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29 results on '"SPITZER"'

1. JWST MIRI/MRS in-flight absolute flux calibration and tailored fringe correction for unresolved sources

Author: Danny Gasman, Ioannis Argyriou, G. C. Sloan, Bernhard Aringer, Javier Álvarez-Márquez, Ori Fox, Alistair Glasse, Adrian Glauser, Olivia C. Jones, Kay Justtanont, Patrick J. Kavanagh, Pamela Klaassen, Alvaro Labiano, Kirsten Larson, David R. Law, Michael Mueller, Omnarayani Nayak, Alberto Noriega-Crespo, Polychronis Patapis, Pierre Royer, and Bart Vandenbussche
Subjects: stars, MODEL ATMOSPHERES, SAMPLE, PARSECS, data analysis, FOS: Physical sciences, Astronomy & Astrophysics, methods, ASTROPY, spectrographs, SPACE-TELESCOPE, infrared: stars, Instrumentation and Methods for Astrophysics (astro-ph.IM), detectors, instrumentation: spectrographs, instrumentation, SPECTRUM, Science & Technology, SPECTROSCOPY, instrumentation: detectors, Astronomy and Astrophysics, methods: data analysis, infrared: stars [instrumentation], LINE LISTS, SPITZER, Space and Planetary Science, Physical Sciences, infrared, Astrophysics - Instrumentation and Methods for Astrophysics, PROJECT
Abstract: Context. The Medium Resolution Spectrometer (MRS) is one of the four observing modes of JWST/MIRI. Using JWST in-flight data of unresolved (point) sources, we can derive the MRS absolute spectral response function (ASRF) starting from raw data. Spectral fringing, caused by coherent reflections inside the detector arrays, plays a critical role in the derivation and interpretation of the MRS ASRF. The fringe corrections implemented in the current pipeline are not optimal for non-extended sources, and a high density of molecular features particularly inhibits an accurate correction. Aims. In this paper, we present an alternative way to calibrate the MIRI/MRS data. Firstly, we derive a fringe correction that accounts for the dependence of the fringe properties on the MIRI/MRS pupil illumination and detector pixel sampling of the point spread function. Secondly, we derive the MRS ASRF using an absolute flux calibrator observed across the full 5- 28 µm wavelength range of the MRS. Thirdly, we apply the new ASRF to the spectrum of a G dwarf and compare it with the output of the JWST/MIRI default data reduction pipeline. Finally, we examine the impact of the different fringe corrections on the detectability of molecular features in the G dwarf and K giant. Methods. The absolute flux calibrator HD 163466 (A-star) was used to derive tailored point source fringe flats at each of the default dither locations of the MRS. The fringe-corrected point source integrated spectrum of HD 163466 was used to derive the MRS ASRF using a theoretical model for the stellar continuum. A cross-correlation was run to quantify the uncertainty on the detection of CO, SiO, and OH in the K giant and CO in the G dwarf for different fringe corrections. Results. The point-source-tailored fringe correction and ASRF are found to perform at the same level as the current corrections, beating down the fringe contrast to the sub-percent level in the G dwarf in the longer wavelengths, whilst mitigating the alteration of real molecular features. The same tailored solutions can be applied to other MRS unresolved targets. Target acquisition is required to ensure the pointing is accurate enough to apply this method. A pointing repeatability issue in the MRS limits the effectiveness of the tailored fringe flats is at short wavelengths. Finally, resulting spectra require no scaling to make the sub-bands match, and a dichroic spectral leak at 12.2 µm is removed., Astronomy & Astrophysics, 673, ISSN:0004-6361, ISSN:1432-0746
Published: 2023

2. Precision measurement of a brown dwarf mass in a binary system in the microlensing event OGLE-2019-BLG-0033/MOA-2019-BLG-035

Author: Herald, A, Udalski, A, Bozza, V, Rota, P, Bond, IA, Yee, JC, Sajadian, S, Mroz, P, Poleski, R, Skowron, J, Szymanski, MK, Soszynski, I, Pietrukowicz, P, Kozlowski, S, Ulaczyk, K, Rybicki, KA, Iwanek, P, Wrona, M, Gromadzki, M, Abe, F, Barry, R, Bennett, DP, Bhattacharya, A, Fukui, A, Fujii, H, Hirao, Y, Itow, Y, Kirikawa, R, Kondo, I, Koshimoto, N, Matsubara, Y, Matsumoto, S, Miyazaki, S, Muraki, Y, Olmschenk, G, Ranc, C, Okamura, A, Rattenbury, NJ, Satoh, Y, Sumi, T, Suzuki, D, Silva, SI, Toda, T, Tristram, PJ, Vandorou, A, Yama, H, Beichman, CA, Bryden, G, Novati, SC, Carey, S, Gaudi, BS, Gould, A, Henderson, CB, Johnson, S, Shvartzvald, Y, Zhu, W, Dominik, M, Hundertmark, M, Jorgensen, UG, Longa-Pena, P, Skottfelt, J, Tregloan-Reed, J, Bach-Moller, N, Burgdorf, M, D'Ago, G, Haikala, L, Hitchcock, J, Khalouei, E, Peixinho, N, Rahvar, S, Snodgrass, C, Southworth, J, Spyratos, P, Zang, W, Yang, H, Mao, S, Bachelet, E, Maoz, D, Street, RA, Tsapras, Y, Christie, GW, Cooper, T, de Almeida, L, Jr, DNJ-D, Green, J, Han, C, Hennerley, S, Marmont, A, McCormick, J, Monard, LAG, Natusch, T, Pogge, R, Collaboration, OGLE, Collaboration, MOA, Team, S, Consortium, M, Collaboration, LCOFUN, European Commission, University of St Andrews. School of Physics and Astronomy, and University of St Andrews. St Andrews Centre for Exoplanet Science
Subjects: GRAVITATIONAL LENS, FOS: Physical sciences, CHEMICAL EVOLUTION, Astrophysics::Cosmology and Extragalactic Astrophysics, GALACTIC BULGE, Q1, general [binaries], QB Astronomy, Astrophysics::Solar and Stellar Astrophysics, PHOTOMETRY, low-mass [stars], QC, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), QB, Earth and Planetary Astrophysics (astro-ph.EP), OPTICAL DEPTH, Astronomy and Astrophysics, 3rd-DAS, PLANET CANDIDATE, Astrophysics - Astrophysics of Galaxies, DIFFERENCE IMAGE-ANALYSIS, SPITZER, low mass [Stars], QC Physics, Astrophysics - Solar and Stellar Astrophysics, GIANT PLANETS, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), DISCOVERY, micro [gravitational lensing], Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Earth and Planetary Astrophysics, brown dwarfs
Abstract: Context. Brown dwarfs are poorly understood transition objects between stars and planets, with several competing mechanisms having been proposed for their formation. Mass measurements are generally difficult for isolated objects but also for brown dwarfs orbiting low-mass stars, which are often too faint for spectroscopic follow-up. Aims. Microlensing provides an alternative tool for the discovery and investigation of such faint systems. Here we present the analysis of the microlensing event OGLE-2019-BLG-0033/MOA-2019-BLG-035, which is due to a binary system composed of a brown dwarf orbiting a red dwarf. Methods. Thanks to extensive ground observations and the availability of space observations from Spitzer, it has been possible to obtain accurate estimates of all microlensing parameters, including parallax, source radius and orbital motion of the binary lens. Results. After accurate modeling, we find that the lens is composed of a red dwarf with mass $M_1 = 0.149 \pm 0.010M_\odot$ and a brown dwarf with mass $M_2 = 0.0463 \pm 0.0031M_\odot$, at a projected separation of $a_\perp = 0.585$ au. The system has a peculiar velocity that is typical of old metal-poor populations in the thick disk. Percent precision in the mass measurement of brown dwarfs has been achieved only in a few microlensing events up to now, but will likely become common with the Roman space telescope., Comment: 13 pages, 6 figures
Published: 2022
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3. B-fields in Star-forming Region Observations (BISTRO): Magnetic Fields in the Filamentary Structures of Serpens Main

Author: Woojin Kwon, Kate Pattle, Sarah Sadavoy, Charles L. H. Hull, Doug Johnstone, Derek Ward-Thompson, James Di Francesco, Patrick M. Koch, Ray Furuya, Yasuo Doi, Valentin J. M. Le Gouellec, Jihye Hwang, A-Ran Lyo, Archana Soam, Xindi Tang, Thiem Hoang, Florian Kirchschlager, Chakali Eswaraiah, Lapo Fanciullo, Kyoung Hee Kim, Takashi Onaka, Vera Könyves, Ji-hyun Kang, Chang Won Lee, Motohide Tamura, Pierre Bastien, Tetsuo Hasegawa, Shih-Ping Lai, Keping Qiu, David Berry, Doris Arzoumanian, Tyler L. Bourke, Do-Young Byun, Wen Ping Chen, Huei-Ru Vivien Chen, Mike Chen, Zhiwei Chen, Tao-Chung Ching, Jungyeon Cho, Yunhee Choi, Minho Choi, Antonio Chrysostomou, Eun Jung Chung, Simon Coudé, Sophia Dai, Pham Ngoc Diep, Yan Duan, Hao-Yuan Duan, David Eden, Jason Fiege, Laura M. Fissel, Erica Franzmann, Per Friberg, Rachel Friesen, Gary Fuller, Tim Gledhill, Sarah Graves, Jane Greaves, Matt Griffin, Qilao Gu, Ilseung Han, Jennifer Hatchell, Saeko Hayashi, Martin Houde, Tsuyoshi Inoue, Shu-ichiro Inutsuka, Kazunari Iwasaki, Il-Gyo Jeong, Miju Kang, Janik Karoly, Akimasa Kataoka, Koji Kawabata, Francisca Kemper, Kee-Tae Kim, Gwanjeong Kim, Mi-Ryang Kim, Shinyoung Kim, Jongsoo Kim, Jason Kirk, Masato I. N. Kobayashi, Takayoshi Kusune, Jungmi Kwon, Kevin Lacaille, Chi-Yan Law, Chin-Fei Lee, Yong-Hee Lee, Hyeseung Lee, Jeong-Eun Lee, Sang-Sung Lee, Dalei Li, Di Li, Hua-bai Li, Sheng-Jun Lin, Sheng-Yuan Liu, Hong-Li Liu, Junhao Liu, Tie Liu, Xing Lu, Steve Mairs, Masafumi Matsumura, Brenda Matthews, Gerald Moriarty-Schieven, Tetsuya Nagata, Fumitaka Nakamura, Hiroyuki Nakanishi, Nguyen Bich Ngoc, Nagayoshi Ohashi, Geumsook Park, Harriet Parsons, Nicolas Peretto, Felix Priestley, Tae-Soo Pyo, Lei Qian, Ramprasad Rao, Jonathan Rawlings, Mark G. Rawlings, Brendan Retter, John Richer, Andrew Rigby, Hiro Saito, Giorgio Savini, Masumichi Seta, Yoshito Shimajiri, Hiroko Shinnaga, Mehrnoosh Tahani, Ya-Wen Tang, Kohji Tomisaka, Le Ngoc Tram, Yusuke Tsukamoto, Serena Viti, Hongchi Wang, Jia-Wei Wang, Anthony Whitworth, Jintai Wu, Jinjin Xie, Hsi-Wei Yen, Hyunju Yoo, Jinghua Yuan, Hyeong-Sik Yun, Tetsuya Zenko, Yapeng Zhang, Chuan-Peng Zhang, Guoyin Zhang, Jianjun Zhou, Lei Zhu, Ilse de Looze, Philippe André, C. Darren Dowell, Stewart Eyres, Sam Falle, Jean-François Robitaille, Sven van Loo, 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), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), and Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France
Subjects: POLARIZATION, FOS: Physical sciences, F500, IMAGING POLARIMETRY, 1ST, INTERSTELLAR CLOUDS, Astrophysics::Solar and Stellar Astrophysics, SCUBA-2, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], LEGACY, Astronomy and Astrophysics, VELOCITY, Astrophysics - Astrophysics of Galaxies, SPITZER, Astrophysics - Solar and Stellar Astrophysics, Physics and Astronomy, Space and Planetary Science, [SDU]Sciences of the Universe [physics], OUTFLOWS, Astrophysics of Galaxies (astro-ph.GA), STRENGTHS
Abstract: We present 850 $��$m polarimetric observations toward the Serpens Main molecular cloud obtained using the POL-2 polarimeter on the James Clerk Maxwell Telescope (JCMT) as part of the B-fields In STar-forming Region Observations (BISTRO) survey. These observations probe the magnetic field morphology of the Serpens Main molecular cloud on about 6000 au scales, which consists of cores and six filaments with different physical properties such as density and star formation activity. Using the histogram of relative orientation (HRO) technique, we find that magnetic fields are parallel to filaments in less dense filamentary structures where $N_{H_2} < 0.93\times 10^{22}$ cm$^{-2}$ (magnetic fields perpendicular to density gradients), while being perpendicular to filaments (magnetic fields parallel to density gradients) in dense filamentary structures with star formation activity. Moreover, applying the HRO technique to denser core regions, we find that magnetic field orientations change to become perpendicular to density gradients again at $N_{H_2} \approx 4.6 \times 10^{22}$ cm$^{-2}$. This can be interpreted as a signature of core formation. At $N_{H_2} \approx 16 \times 10^{22}$ cm$^{-2}$ magnetic fields change back to being parallel to density gradients once again, which can be understood to be due to magnetic fields being dragged in by infalling material. In addition, we estimate the magnetic field strengths of the filaments ($B_{POS} = 60-300~��$G)) using the Davis-Chandrasekhar-Fermi method and discuss whether the filaments are gravitationally unstable based on magnetic field and turbulence energy densities., 18 pages, accepted for publication in ApJ
Published: 2022
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4. K2 and Spitzer phase curves of the rocky ultra-short-period planet K2-141 b hint at a tenuous rock vapor atmosphere

Author: Zieba, Sebastian, Zilinskas, Mantas, Kreidberg, Laura, Nguyen, T. Giang, Miguel, Yamila, Cowan, Nicolas B., Pierrehumbert, Raymond, Carone, Ludmila, Dang, Lisa, Hammond, Mark, Louden, Tom, Lupu, Roxana, Malavolta, Luca, and Stevenson, Kevin B.
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Planets and satellites: individual: K2-141 b, Spitzer, planets and satellites: atmospheres, planets and satellites: individual: K2-141 b, techniques: photometric, Exoplanets, K2-141 b, lava planet, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Space and Planetary Science, atmospheres, Astrophysics::Solar and Stellar Astrophysics, Planets and satellites: atmospheres, Astrophysics::Earth and Planetary Astrophysics, Techniques: photometric, Astrophysics - Earth and Planetary Astrophysics
Abstract: K2-141 b is a transiting, small (1.5 Re) ultra-short-period (USP) planet discovered by Kepler orbiting a K-dwarf host star every 6.7 hours. The planet's high surface temperature makes it an excellent target for thermal emission observations. Here we present 65 hours of continuous photometric observations of K2-141 b collected with Spitzer's IRAC Channel 2 at 4.5 micron spanning 10 full orbits of the planet. We measure an infrared eclipse depth of 143 +/- 39 ppm and a peak to trough amplitude variation of 121 +/- 43 ppm. The best fit model to the Spitzer data shows no significant thermal hotspot offset, in contrast to the previously observed offset for the well-studied USP planet 55 Cnc e. We also jointly analyze the new Spitzer observations with the photometry collected by Kepler during two separate K2 campaigns. We model the planetary emission with a range of toy models that include a reflective and a thermal contribution. With a two-temperature model, we measure a dayside temperature of 2049 +/- 361 K and a night-side temperature that is consistent with zero (Tp,n < 1712 K at 2 sigma). Models with a steep dayside temperature gradient provide a better fit to the data than a uniform dayside temperature (DeltaBIC = 22.2). We also find evidence for a non-zero geometric albedo Ag = 0.28 +/- 0.07. We also compare the data to a physically motivated, pseudo-2D rock vapor model and a 1D turbulent boundary layer model. Both models fit the data well. Notably, we find that the optical eclipse depth can be explained by thermal emission from a hot inversion layer, rather than reflected light. A thermal inversion may also be responsible for the deep optical eclipse observed for another USP, Kepler-10 b. Finally, we significantly improve the ephemerides for K2-141 b and c, which will facilitate further follow-up observations of this interesting system with state-of-the-art observatories like JWST., 31 pages, 27 figures, 12 tables, accepted for publication in A&A
Published: 2022

5. A First Look into the Nature of JWST/MIRI 7.7 μm Sources from SMACS 0723

Author: Edoardo Iani, Karina I. Caputi, Pierluigi Rinaldi, Vasily I. Kokorev, and Astronomy
Subjects: LEGACY, FOS: Physical sciences, Astronomy and Astrophysics, I, FIELDS, Astrophysics - Astrophysics of Galaxies, EVOLUTION, GALAXIES, SPITZER, SPACE-TELESCOPE OBSERVATIONS, STELLAR, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), PHOTOMETRY, PROJECT
Abstract: Until now, our knowledge of the extragalactic Universe at mid-IR wavelengths (> 5 microns) was limited to rare active galactic nuclei (AGN) and the brightest normal galaxies up to z~3. The advent of the JWST with its Mid-Infrared Instrument (MIRI) will revolutionise the ability of the mid-IR regime as a key wavelength domain to probe the high-z Universe. In this work we present a first study of JWST MIRI 7.7 micron sources selected with > 3 sigma significance from the lensing cluster field SMACS J0723.3-7327. We model their spectral energy distribution fitting with 13 JWST and HST broad bands, in order to obtain photometric redshifts and derived physical parameters for all these sources. We find that this 7.7 micron galaxy sample is mainly composed of normal galaxies up to z=4 and has a tail of about 2% of sources at higher redshifts to z~ 9-10. The vast majority of our galaxies have [3.6]-[7.7], 13 pages, 9 figures, 2 tables. Accepted for publication at the ApJ. In the current version we make the 7.7 micron source catalogue publicly available
Published: 2022
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6. GOODS-ALMA: Using IRAC and VLA to probe fainter millimeter galaxies

Author: Neil M. Nagar, M. Franco, Maurilio Pannella, C. Gómez-Guijarro, Laure Ciesla, E. Daddi, Casey Papovich, Stéphanie Juneau, Koryo Okumura, Henry C. Ferguson, Matthieu Béthermin, David Elbaz, Lihwai Lin, Mark Dickinson, Frédéric Bournaud, Mauro Giavalisco, Tao Wang, John D. Silverman, Steven L. Finkelstein, Hanae Inami, L. Zhou, Xinwen Shu, R. T. Coogan, Benjamin Magnelli, Kentaro Motohara, Daisuke Iono, Guilaine Lagache, Georgios E. Magdis, Wiphu Rujopakarn, Alexandra Pope, Corentin Schreiber, Mengyuan Xiao, David M. Alexander, Ricardo Demarco, James Mullaney, Ranga-Ram Chary, Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), University of Hertfordshire [Hatfield] (UH), Nanjing University (NJU), Argelander Institute for Astronomy (AlfA), Rheinische Friedrich-Wilhelms-Universität Bonn, University of Oxford, 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), National Optical Astronomy Observatory (NOAO), Universidad de Conception, Niels Bohr Institute [Copenhagen] (NBI), Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH), National Observatory of Athens (NOA), Durham University, University of Sheffield [Sheffield], Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Hiroshima University, Anhui Normal University, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Infrared Processing and Analysis Center (IPAC), California Institute of Technology (CALTECH), Max Planck Institute for Extraterrestrial Physics (MPE), Max-Planck-Gesellschaft, Space Telescope Science Institute (STSci), University of Texas at Austin [Austin], University of Massachusetts [Amherst] (UMass Amherst), University of Massachusetts System (UMASS), National Astronomical Observatory of Japan (NAOJ), Graduate University for Advanced Studies [Hayama] (SOKENDAI), Università degli studi di Trieste = University of Trieste, Ludwig-Maximilians-Universität München (LMU), Kavli Institute for the Physics and Mathematics of the Universe [Tokyo] (Kavli IPMU), The University of Tokyo Institutes for Advanced Study (UTIAS), The University of Tokyo (UTokyo)-The University of Tokyo (UTokyo), Chulalongkorn University [Bangkok], National Astronomical Research Institute of Thailand (NARIT), This work was supported by the Programme National Cosmology et Galaxies (PNCG) of CNRS/INSU with INP and IN2P3, co-funded by CEA and CNES., European Project: 648179,H2020,ERC-2014-CoG,ConTExt(2015), European Project: 716762,ClustersXCosmo, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), University of Oxford [Oxford], University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), and University of Trieste
Subjects: submillimeter: galaxies, SPECTROSCOPIC SURVEY, TELESCOPE, IMAGER, SCUBA, FOS: Physical sciences, CAMERA, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, star formation [Galaxies], 01 natural sciences, high-redshift [Galaxies], galaxies [Submillimeter], galaxies: high-redshift, 0103 physical sciences, STAR-FORMING GALAXIES, Astrophysics::Solar and Stellar Astrophysics, FIELD, 010303 astronomy & astrophysics, License, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, photometry [Galaxies], Astronomy and Astrophysics, galaxies: fundamental parameters, Creative commons, evolution [Galaxies], Astrophysics - Astrophysics of Galaxies, Galaxy, SPITZER, galaxies: photometry, ORIGINS DEEP SURVEY, STELLAR, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), galaxies: star formation, fundamental parameters [Galaxies], Millimeter, Astrophysics::Earth and Planetary Astrophysics, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: In this paper, we extend the source detection in the GOODS-ALMA field (69 arcmin$^2$, rms sensitivity $\sigma$ $\simeq$ 0.18 mJy.beam$^{-1}$), to deeper levels than presented in Franco et al. (2018). Using positional information at 3.6 and 4.5 $\mu$m (from Spitzer-IRAC), we explore the presence of galaxies detected at 1.1 mm with ALMA below our original blind detection limit of 4.8-$\sigma$ at which the number of spurious sources starts to dominate over that of real sources. In this Supplementary Catalog, we find a total of 16 galaxies, including 2 galaxies with no counterpart in HST images (also known as optically-dark galaxies) down to a 5$\sigma$ limiting depth of H = 28.2 AB (HST/WFC3 F160W). This brings the total sample of GOODS-ALMA 1.1 mm sources to 35 galaxies. Galaxies in the new sample cover a wider dynamic range in redshift ($z$ = 0.65 - 4.73), are on average twice as large (1.3 vs 0.65 kpc) and and have lower stellar mass (M$_{\star}^{\rm SC}$ = 7.6$\times$10$^{10}$M$_\odot$ vs M$_{\star}^{\rm MC}$ = 1.2$\times$10$^{11}$M$_\odot$). Although exhibiting larger physical sizes, these galaxies have still far-infrared sizes significantly more compact than inferred from their optical emission. We show that the astrometry of the HST image does not only suffer from a global astrometric shift, as already discussed in previous papers, but also from local shifts. These distortions were artificially introduced in the process of building the mosaic of the GOODS-South HST image. By comparing the positions of almost 400 galaxies detected by HST, Pan-STARRS and ALMA, we create a distortion map which can be used to correct for these astrometric issues., Comment: 18 pages, 13 figures. Accepted for publication in A&A
Published: 2020
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7. Have we seen all the galaxies that comprise the cosmic infrared background at 250 μm ≤ λ ≤ 500 μm?

Author: Peter Hurley, Douglas Scott, Rob Ivison, Matthieu Béthermin, Michael Zemcov, S. Duivenvoorden, R. Shirley, Lingyu Wang, Duncan Farrah, G. de Zotti, David L. Clements, S. J. Oliver, Andreas Efstathiou, Guilaine Lagache, 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), Astronomy, Science and Technology Facilities Council (STFC), Imperial College Trust, and Science and Technology Facilities Council
Subjects: Population, Astrophysics, Large Synoptic Survey Telescope, Astronomy & Astrophysics, DEG(2), 01 natural sciences, STAR-FORMATION, infrared: galaxies, Cosmic infrared background, 0201 Astronomical and Space Sciences, 0103 physical sciences, education, 010303 astronomy & astrophysics, QC, Luminous infrared galaxy, Physics, LEGACY SURVEY, education.field_of_study, Science & Technology, COSMIC cancer database, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Star formation, Astronomy and Astrophysics, Galaxy, EVOLUTION, Wavelength, SPITZER, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Physical Sciences, HELP, submillimetre: galaxies
Abstract: International audience; The cosmic infrared background (CIB) provides a fundamental observational constraint on the star formation history of galaxies over cosmic history. We estimate the contribution to the CIB from catalogued galaxies in the COSMOS field by using a novel map fitting technique on the Herschel SPIRE maps. Prior galaxy positions are obtained using detections over a large range in wavelengths in the Ks-3 GHz range. Our method simultaneously fits the galaxies, the system foreground, and the leakage of flux from galaxies located in masked areas and corrects for an 'overfitting' effect not previously accounted for in stacking methods. We explore the contribution to the CIB as a function of galaxy survey wavelength and depth. We find high contributions to the CIB with the deep r (mAB ≤ 26.5), Ks (mAB ≤ 24.0), and 3.6 μm (mAB ≤ 25.5) catalogues. We combine these three deep catalogues and find a total CIB contributions of 10.5 ± 1.6, 6.7 ± 1.5, and 3.1 ± 0.7 nWm-2 sr-1 at 250, 350, and 500 μm, respectively. Our CIB estimates are consistent with recent phenomenological models, prior based SPIRE number counts and with (though more precise than) the diffuse total measured by FIRAS. Our results raise the interesting prospect that the CIB contribution at λ ≤ 500 μm from known galaxies has converged. Future large-area surveys like those with the Large Synoptic Survey Telescope are therefore likely to resolve a substantial fraction of the population responsible for the CIB at 250 μm ≤ λ ≤ 500 μm.
Published: 2020
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8. Dust evolution across the Horsehead nebula

Author: Mika Juvela, Alain Abergel, Anthony P. Jones, T. Schirmer, Laurent Verstraete, Emilie Habart, Nathalie Ysard, Service d'Hépatologie Gastro-entérologie [CHU Clermont-Ferrand], CHU Estaing [Clermont-Ferrand], CHU Clermont-Ferrand-CHU Clermont-Ferrand, 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), University of Helsinki, and Department of Physics
Subjects: 010504 meteorology & atmospheric sciences, Extinction (astronomy), FOS: Physical sciences, Context (language use), Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, PHOTODISSOCIATION REGIONS, 01 natural sciences, STAR-FORMATION, photon-dominated region, evolution, 0103 physical sciences, SIZE DISTRIBUTION, Radiative transfer, Astrophysics::Solar and Stellar Astrophysics, COLD DUST, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Cosmic dust, Physics, Nebula, extinction, Star formation, Scattering, Astronomy and Astrophysics, 115 Astronomy, Space science, Astrophysics - Astrophysics of Galaxies, Interstellar medium, SPITZER, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), MULTIBAND IMAGING PHOTOMETER, ISM: individual objects: Horsehead nebula, Astrophysics::Earth and Planetary Astrophysics, dust, EMISSION, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], ABSOLUTE CALIBRATION, INTERSTELLAR DUST
Abstract: Context. Micro-physical processes on interstellar dust surfaces are tightly connected to dust properties (i.e. dust composition, size, and shape) and play a key role in numerous phenomena in the interstellar medium (ISM). The large disparity in physical conditions (i.e. density and gas temperature) in the ISM triggers an evolution of dust properties. The analysis of how dust evolves with the physical conditions is a stepping stone towards a more thorough understanding of interstellar dust. Aims. We highlight dust evolution in the Horsehead nebula photon-dominated region. Methods. We used Spitzer/IRAC (3.6, 4.5, 5.8 and 8 μm) and Spitzer/MIPS (24 μm) together with Herschel/PACS (70 and 160 μm) and Herschel/SPIRE (250, 350 and 500 μm) to map the spatial distribution of dust in the Horsehead nebula over the entire emission spectral range. We modelled dust emission and scattering using the THEMIS interstellar dust model together with the 3D radiative transfer code SOC. Results. We find that the nano-grain dust-to-gas ratio in the irradiated outer part of the Horsehead is 6–10 times lower than in the diffuse ISM. The minimum size of these grains is 2–2.25 times larger than in the diffuse ISM, and the power-law exponent of their size distribution is 1.1–1.4 times lower than in the diffuse ISM. In the denser part of the Horsehead nebula, it is necessary to use evolved grains (i.e. aggregates, with or without an ice mantle). Conclusions. It is not possible to explain the observations using grains from the diffuse medium. We therefore propose the following scenario to explain our results. In the outer part of the Horsehead nebula, all the nano-grain have not yet had time to re-form completely through photo-fragmentation of aggregates and the smallest of the nano-grain that are sensitive to the radiation field are photo-destroyed. In the inner part of the Horsehead nebula, grains most likely consist of multi-compositional mantled aggregates.
Published: 2020
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9. The dust content of the Crab Nebula

Author: I. De Looze, F. D. Priestley, A. Bevan, M. J. Barlow, Mikako Matsuura, Haley Louise Gomez, Michael Bietenholz, Rino Bandiera, H. Chawner, Roger Wesson, ITA, GBR, BEL, CAN, and ZAF
Subjects: Astrophysics::High Energy Astrophysical Phenomena, MAGNETOHYDRODYNAMIC SIMULATIONS, Extinction (astronomy), individual: Crab Nebula [supernovae], Flux, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Pulsar, INTERSTELLAR SILICATE MINERALOGY, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, SPACE, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Cosmic dust, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Spectral index, 010308 nuclear & particles physics, supernova remnants [ISM], Astronomy and Astrophysics, non-thermal [radiation mechanisms], Astrophysics - Astrophysics of Galaxies, Galaxy, EVOLUTION, Supernova, SPITZER, CASSIOPEIA, Crab Nebula, Physics and Astronomy, Space and Planetary Science, SUPERNOVA REMNANT, Astrophysics of Galaxies (astro-ph.GA), MULTIBAND IMAGING PHOTOMETER, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, PULSAR-WIND NEBULAE, ABSOLUTE CALIBRATION
Abstract: We have modelled the near-infrared to radio images of the Crab Nebula with a Bayesian SED model to simultaneously fit its synchrotron, interstellar and supernova dust emission. We infer an interstellar dust extinction map with an average $A_{\text{V}}$=1.08$\pm$0.38 mag, consistent with a small contribution (, Comment: 33 pages, 17 figures, Manuscript accepted for publication in MNRAS. Accepted on 31/05/2019. Deposited on 31/05/2019
Published: 2019

10. HFF-DeepSpace photometric catalogs of the 12 Hubble frontier fields, clusters, and parallels: photometry, photometric redshifts, and stellar masses

Author: Rosalind E. Skelton, Heath Shipley, Laura Ferrarese, Kalina V. Nedkova, Adina D. Feinstein, Erin Kado-Fong, Nicholas Martis, Mauro Stefanon, Katherine E. Whitaker, Danilo Marchesini, Daniel Lange-Vagle, Arjen van der Wel, Britt Lundgren, Ivo Labbé, Adam Muzzin, Gabriel B. Brammer, and Pascal Oesch
Subjects: DEPENDENT EVOLUTION, Hubble Deep Field, POPULATION SYNTHESIS, PROPAGATION, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Advanced Camera for Surveys, galaxies [infrared], GALAXY CLUSTER, UNCERTAINTIES, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, DEEP-FIELD, 010303 astronomy & astrophysics, Galaxy cluster, evolution [galaxies], Astrophysics::Galaxy Astrophysics, STAR-FORMATION HISTORIES, Luminous infrared galaxy, Physics, Very Large Telescope, FORMING GALAXIES, 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, First light, Redshift, SPITZER, Physics and Astronomy, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, MULTIPLE IMAGES, Wide Field Camera 3, high-redshift [galaxies]
Abstract: We present Hubble multi-wavelength photometric catalogs, including (up to) 17 filters with the Advanced Camera for Surveys and Wide Field Camera 3 from the ultra-violet to near-infrared for the Hubble Frontier Fields and associated parallels. We have constructed homogeneous photometric catalogs for all six clusters and their parallels. To further expand these data catalogs, we have added ultra-deep K S -band imaging at 2.2 μm from the Very Large Telescope HAWK-I and Keck-I MOSFIRE instruments. We also add post-cryogenic Spitzer imaging at 3.6 and 4.5 μm with the Infrared Array Camera (IRAC), as well as archival IRAC 5.8 and 8.0 μm imaging when available. We introduce the public release of the multi-wavelength (0.2-8 μm) photometric catalogs, and we describe the unique steps applied for the construction of these catalogs. Particular emphasis is given to the source detection band, the contamination of light from the bright cluster galaxies (bCGs), and intra-cluster light (ICL). In addition to the photometric catalogs, we provide catalogs of photometric redshifts and stellar population properties. Furthermore, this includes all the images used in the construction of the catalogs, including the combined models of bCGs and ICL, the residual images, segmentation maps, and more. These catalogs are a robust data set of the Hubble Frontier Fields and will be an important aid in designing future surveys, as well as planning follow-up programs with current and future observatories to answer key questions remaining about first light, reionization, the assembly of galaxies, and many more topics, most notably by identifying high-redshift sources to target.
Published: 2018

11. SPICA —A Large Cryogenic Infrared Space Telescope: Unveiling the Obscured Universe

Author: M. Kawada, B. Larsson, D. Arrazola, Brian Jackson, C.M. Bradford, Lee Armus, K. Shinozaki, Hiroshi Shibai, Francisca Kemper, N. Isobe, I. Funaki, R. Huisman, M. Giard, L. Duband, Shiang-Yu Wang, P. Khosropanah, Shinki Oyabu, P. P. Kooijman, R. Shipman, Daisuke Ishihara, I. Charles, L. Rodriguez, V. Reveret, S. Withington, Frank Helmich, Kotaro Kohno, Willem Jellema, Pieter Dieleman, M. Audard, T. Wada, B. Vandenbussche, D. van Loon, A. Di Giorgio, Peter Roelfsema, David A. Naylor, I. Sakon, H. Ogawa, G. de Lange, Franz Kerschbaum, J. Kwon, R. Hijmering, W. M. Laauwen, J. van der Kuur, Jaap Evers, Francisco Najarro, Inga Kamp, Takashi Onaka, Albrecht Poglitsch, T. Yamada, L. M. González Fernández, H. Jacobs, S. C. Madden, Hidehiro Kaneda, Yasuo Doi, Jian-Rong Gao, C. K. Wafelbakker, H. van Weers, M. Eggens, I. Yamamura, L. Spinoglio, H. Matsuhara, Oliver Krause, T. Suzuki, Takao Nakagawa, Matthew Joseph Griffin, F. F. S. van der Tak, H. Sugita, Michael D. Audley, Y. Sato, J. Torres Redondo, 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), ISDC Data Centre for Astrophysics, University of Geneva [Switzerland], Institut Nanosciences et Cryogénie (INAC), Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Massachusetts Institute of Technology (MIT), inconnu, Inconnu, Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA), School of Physics and Astronomy [Cardiff], Cardiff University, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Kapteyn Astronomical Institute [Groningen], University of Groningen [Groningen], AUTRES, National Institute for Subatomic Physics [Amsterdam] (NIKHEF), 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), Departamento de Astrofisica [Madrid], Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Department of Physics, Nara Women's University, Department of Environmental and Materials Engineering, Nagoya Institute, Max-Planck-Institut für Extraterrestrische Physik (MPE), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Antarctic Research a European Network for Astrophysics (ARENA), Nanomaterials Research Institute, foreign laboratories (FL), CERN [Genève], SRON Netherlands Institute for Space Research (SRON), Instituut voor Sterrenkunde [Leuven], Catholic University of Leuven - Katholieke Universiteit Leuven (KU Leuven), NASA Goddard Space Flight Center (GSFC), Astronomy, Université de Genève = University of Geneva (UNIGE), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), 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), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes (UGA), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Université Côte d'Azur (UCA), Laboratoire d'Astrophysique de Grenoble (LAOG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), National Institute for Subatomic Physics Nikhef [Amsterdam] (NIKHEF), and Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA)
Subjects: infrared: galaxies, infrared: general, infrared: planetary systems, instrumentation: photometers, instrumentation: spectrographs, space vehicles: instruments, Astrophysics - Instrumentation and Methods for Astrophysics, instruments [space vehicles], Direct assessment, Infrared, media_common.quotation_subject, Infrared wavelength, FOS: Physical sciences, Spica, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, Space (mathematics), 01 natural sciences, galaxies [infrared], infrared: galaxies, Spitzer Space Telescope, 0103 physical sciences, photometers [instrumentation], space vehicles: instruments, 010306 general physics, infrared: planetary systems, planetary systems [infrared], Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, general [infrared], Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, media_common, instrumentation: spectrographs, MISSION, Luminous infrared galaxy, Physics, Science & Technology, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, Universe, instrumentation: photometers, SPITZER, Space and Planetary Science, Physical Sciences, Astrophysics::Earth and Planetary Astrophysics, infrared: general, Astrophysics - Instrumentation and Methods for Astrophysics, spectrographs [instrumentation]
Abstract: 著者人数: 70名(所属. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS): 芝井, 広; 船木, 一幸; 磯部, 直樹; 川田, 光伸; 權, 靜美; 松原, 英雄; 中川, 貴雄; 小川, 博之; 佐藤, 洋一; 篠崎, 慶亮; 杉田, 寛之; 和田, 武彦; 山田, 亨; 山村, 一誠), Number of authors: 70(Affiliation. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA)(ISAS): Shibai, Hiroshi; Funaki, Ikkoh; Isobe, Naoki; Kawada, Mitsunobu; Kwon, Jungmi; Matsuhara, Hideo; Nakagawa, Takao; Ogawa, Hiroyuki; Sato, Yoichi; Shinozaki, Keisuke; Sugita, Hiroyuki; Wada, Takehiko; Yamada, Toru; Yamamura, Issei), 資料番号: SA1180106000
Published: 2018
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12. De‐blending deep Herschel surveys: A multi‐wavelength approach

Author: F. F. S. van der Tak, Lingyu Wang, W. J. Pearson, S. J. Oliver, Peter Hurley, Denis Burgarella, 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), Astronomy, 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: Gaussian, INFRARED-EMISSION, FOS: Physical sciences, Flux, HERMES, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Standard deviation, infrared: galaxies, Photometry (optics), symbols.namesake, 0103 physical sciences, Prior probability, STAR-FORMING GALAXIES, PHOTOMETRY, 010303 astronomy & astrophysics, galaxies: statistics, Astrophysics::Galaxy Astrophysics, COSMOS, Physics, Luminous infrared galaxy, ALMA OBSERVATIONS, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Spectral density, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, SPITZER, STELLAR, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), symbols, CONFUSION, INTERSTELLAR DUST
Abstract: Cosmological surveys in the far infrared are known to suffer from confusion. The Bayesian de-blending tool, XID+, currently provides one of the best ways to de-confuse deep Herschel SPIRE images, using a flat flux density prior. This work is to demonstrate that existing multi-wavelength data sets can be exploited to improve XID+ by providing an informed prior, resulting in more accurate and precise extracted flux densities. Photometric data for galaxies in the COSMOS field were used to constrain spectral energy distributions (SEDs) using the fitting tool CIGALE. These SEDs were used to create Gaussian prior estimates in the SPIRE bands for XID+. The multi-wavelength photometry and the extracted SPIRE flux densities were run through CIGALE again to allow us to compare the performance of the two priors. Inferred ALMA flux densities (F$^i$), at 870$\mu$m and 1250$\mu$m, from the best fitting SEDs from the second CIGALE run were compared with measured ALMA flux densities (F$^m$) as an independent performance validation. Similar validations were conducted with the SED modelling and fitting tool MAGPHYS and modified black body functions to test for model dependency. We demonstrate a clear improvement in agreement between the flux densities extracted with XID+ and existing data at other wavelengths when using the new informed Gaussian prior over the original uninformed prior. The residuals between F$^m$ and F$^i$ were calculated. For the Gaussian prior, these residuals, expressed as a multiple of the ALMA error ($\sigma$), have a smaller standard deviation, 7.95$\sigma$ for the Gaussian prior compared to 12.21$\sigma$ for the flat prior, reduced mean, 1.83$\sigma$ compared to 3.44$\sigma$, and have reduced skew to positive values, 7.97 compared to 11.50. These results were determined to not be significantly model dependent. This results in statistically more reliable SPIRE flux densities., Comment: 8 pages, 7 figures, 3 tables. Accepted for publication in A&A
Published: 2017
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13. Infrared Emission by Dust Around λ Bootis Stars

Author: Juan Rafael Martínez-Galarza, George H. Rieke, Eric E. Mamajek, Inga Kamp, Kate Y. L. Su, Andras Gaspar, and Astronomy
Subjects: Infrared, A-STARS, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Lambda, circumstellar matter, ISM: clouds, SOLAR-SYSTEM, PARTICLE-TRANSPORT, Astrophysics::Solar and Stellar Astrophysics, ACCRETION, Astrophysics::Galaxy Astrophysics, Physics, infrared: ISM, Photosphere, Debris disk, Astrophysics (astro-ph), Astronomy and Astrophysics, MASS-LOSS, HI CLOUDS, DIFFUSE INTERSTELLAR-MEDIUM, Accretion (astrophysics), stars: chemically peculiar, Stars, SPITZER, Local Bubble, Radiation pressure, Space and Planetary Science, MULTIBAND IMAGING PHOTOMETER, Astrophysics::Earth and Planetary Astrophysics, ABSOLUTE CALIBRATION
Abstract: We present a model that describes stellar infrared excesses due to heating of the interstellar (IS) dust by a hot star passing through a diffuse IS cloud. This model is applied to six lambda Bootis stars with infrared excesses. Plausible values for the IS medium (ISM) density and relative velocity between the cloud and the star yield fits to the excess emission. This result is consistent with the diffusion/accretion hypothesis that lambda Bootis stars (A- to F-type stars with large underabundances of Fe-peak elements) owe their characteristics to interactions with the ISM. This proposal invokes radiation pressure from the star to repel the IS dust and excavate a paraboloidal dust cavity in the IS cloud, while the metal-poor gas is accreted onto the stellar photosphere. However, the measurements of the infrared excesses can also be fit by planetary debris disk models. A more detailed consideration of the conditions to produce lambda Bootis characteristics indicates that the majority of infrared-excess stars within the Local Bubble probably have debris disks. Nevertheless, more distant stars may often have excesses due to heating of interstellar material such as in our model., 10 pages, 5 figures, 4 tables, accepted by ApJ, emulateapj
Published: 2009

14. Cold galaxies

Author: Michael Rowan-Robinson, David L. Clements, Science and Technology Facilities Council (STFC), and Science and Technology Facilities Council [2006-2012]
Subjects: astro-ph.GA, FOS: Physical sciences, galaxies: starburst, DUST, HERMES, Astrophysics, SPECTRAL ENERGY-DISTRIBUTIONS, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, Luminosity, infrared: galaxies, symbols.namesake, SEDS, Angular diameter, Astrophysics::Solar and Stellar Astrophysics, Surface brightness, Planck, PHOTOMETRIC REDSHIFTS, Astrophysics::Galaxy Astrophysics, Physics, HERSCHEL, Science & Technology, stars: formation, IDENTIFICATION, Radiation field, Spectral density, Astronomy and Astrophysics, CATALOG, Astrophysics - Astrophysics of Galaxies, Galaxy, SPITZER, 0201 Astronomical And Space Sciences, Space and Planetary Science, cosmology: observations, Astrophysics of Galaxies (astro-ph.GA), Physical Sciences, symbols, Astrophysics::Earth and Planetary Astrophysics, galaxies: evolution
Abstract: We use 350 mu angular diameter estimates from Planck to test the idea that some galaxies contain exceptionally cold (10-13 K) dust, since colder dust implies a lower surface brightness radiation field illuminating the dust, and hence a greater physical extent for a given luminosity. The galaxies identified from their spectral energy distributions as containing cold dust do indeed show the expected larger 350 mu diameters. For a few cold dust galaxies where Herschel data are available we are able to use submillimetre maps or surface brightness profiles to locate the cold dust, which as expected generally lies outside the optical galaxy., Comment: 9 pages, 15 figures. Accepted for publication MNRAS
Published: 2015
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15. Extreme conditions in a close analog to the young solar system : Herschel observations of ε Eridani

Author: E. E. Pantin, B. L. de Vries, René Liseau, Göran Pilbratt, Walter Kieran Gear, W. R. F. Dent, Brenda C. Matthews, Bram Acke, Carsten Dominik, Alexis Brandeker, George J. Bendo, Bart Vandenbussche, J. Di Francesco, Rob Ivison, G. Olofsson, Bruce Sibthorpe, Malcolm Fridlund, Michiel R. Hogerheijde, Jane Greaves, M. J. Barlow, J. A. D. L. Blommaert, Paul M. Harvey, Wayne S. Holland, H. J. Walker, C. Waelkens, Science & Technology Facilities Council, University of St Andrews. School of Physics and Astronomy, and Low Energy Astrophysics (API, FNWI)
Subjects: Brightness, Solar System, Spitzer, Evolution, Astronomy, Belt, stars: individual (ε Eridani), Vega, Planets, circumstellar matter, Astrophysics, Star epison-eridani, Planet, QB Astronomy, GeneralLiterature_REFERENCE(e.g.,dictionaries,encyclopedias,glossaries), Migration, QC, circumstellar matter: planet–disk interactions, QB, Physics, Debris disk, planet-disk interactions, Research Programm of Institute for Mathematics, Astrophysics and Particle Physics, Astronomy and Astrophysics, Circumstellar matter, Mass, individual (is an element of Eridani) [Stars], Stars, QC Physics, Devris disk, Space and Planetary Science, Asteroid, Size distributions, stars: individual: epsilon Eridani, Circumstellar habitable zone, Main sequence, Planet-disk interactions
Abstract: Far-infrared Herschel images of the is an element of Eridani system, seen at a fifth of the Sun's present age, resolve two belts of debris emission. Fits to the 160 mu m PACS image yield radial spans for these belts of 12-16 and 54-68 AU. The south end of the outer belt is approximate to 10% brighter than the north end in the PACS+SPIRE images at 160, 250, and 350 mu m, indicating a pericenter glow attributable to a planet "c" From this asymmetry and an upper bound on the offset of the belt center, this second planet should be mildly eccentric (e(c) approximate to 0.03-0.3). Compared to the asteroid and Kuiper Belts of the young Sun, the is an element of Eri belts are intermediate in brightness and more similar to each other, with up to 20 km sized collisional fragments in the inner belt totaling approximate to 5% of an Earth mass. This reservoir may feed the hot dust close to the star and could send many impactors through the Habitable Zone, especially if it is being perturbed by the suspected planet is an element of Eri b, at semi-major axis approximate to 3 AU.
Published: 2014

16. WISE detections of known QSOs at redshifts greater than six

Author: Roc M. Cutri, Carrie Bridge, Chao-Wei Tsai, Robert Assef, Sara Petty, Thomas H. Jarrett, Dominic J. Benford, Jingwen Wu, Andrew Blain, Daniel Stern, Peter Eisenhardt, Ned Wright, Department of Astronomy, and Faculty of Science
Subjects: QSOS, z quasar survey, Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, galaxies: active, FOS: Physical sciences, z-greater-than-5.7 quasars, Astrophysics, Article, infrared: galaxies, additional quasars, midinfrared selection, media_common, Physics, quasars, Astronomy and Astrophysics, z-similar-to-6 quasars, spitzer, Redshift, energy-distributions, observations, Space and Planetary Science, Sky, general, active galactic nuclei, spectral, digital sky survey, galaxies: evolution, host galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present WISE All-Sky mid-infrared (IR) survey detections of 55% (17/31) of the known QSOs at z>6 from a range of surveys: the SDSS, the CFHT-LS, FIRST, Spitzer and UKIDSS. The WISE catalog thus provides a substantial increase in the quantity of IR data available for these sources: 17 are detected in the WISE W1 (3.4-micron) band, 16 in W2 (4.6-micron), 3 in W3 (12-micron) and 0 in W4 (22-micron). This is particularly important with Spitzer in its warm-mission phase and no faint follow-up capability at wavelengths longwards of 5 microns until the launch of JWST. WISE thus provides a useful tool for understanding QSOs found in forthcoming large-area optical/IR sky surveys, using PanSTARRS, SkyMapper, VISTA, DES and LSST. The rest-UV properties of the WISE-detected and the WISE-non-detected samples differ: the detections have brighter i/z-band magnitudes and redder rest-UV colors. This suggests that a more aggressive hunt for very-high-redshift QSOs, by combining WISE W1 and W2 data with red observed optical colors could be effective at least for a subset of dusty candidate QSOs. Stacking the WISE images of the WISE-non-detected QSOs indicates that they are on average significantly fainter than the WISE-detected examples, and are thus not narrowly missing detection in the WISE catalog. The WISE-catalog detection of three of our sample in the W3 band indicates that their mid-IR flux can be detected individually, although there is no stacked W3 detection of sources detected in W1 but not W3. Stacking analyses of WISE data for large AGN samples will be a useful tool, and high-redshift QSOs of all types will be easy targets for JWST., 7 pages; 6 figures; in press at ApJ
Published: 2013
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17. Herschel-ATLAS: Planck sources in the phase 1 fields

Author: Andrea Lapi, Giulia Rodighiero, Matt J. Jarvis, A. Cooray, George J. Bendo, Loretta Dunne, S. Buttiglione, Luigi Danese, Edo Ibar, Francisco J. Carrera, Douglas Scott, Maarten Baes, Stephen Anthony Eales, Laura Bonavera, Rob Ivison, Herve Dole, Michał J. Michałowski, Carlos D. Hoyos, David L. Clements, Marcel Clemens, P. van der Werf, G. de Zotti, D. Herranz, J. González-Nuevo, A. Dariush, Hai Fu, Guilaine Lagache, Steve Maddox, M. López-Caniego, Ivan Valtchanov, Robbie Richard Auld, Mattia Negrello, Marcella Massardi, R. Hopwood, E. E. Rigby, Elisabetta Valiante, Science and Technology Facilities Council (STFC), Science and Technology Facilities Council [2006-2012], Universidad de Cantabria, Ministerio de Ciencia e Innovación (España), Ministerio de Educación, Cultura y Deporte (España), European Commission, and Istituto Nazionale di Fisica Nucleare
Subjects: submillimeter: galaxies, SAMPLE, galaxies [submillimeter], Astrophysics, SUBMILLIMETER GALAXY, Physics, DETECTIONS, COUNTS, INSTRUMENT, gravitational lensing: strong, medicine.anatomical_structure, strong [gravitational lensing], Physical Sciences, symbols, astro-ph.CO, Infrared: galaxies, Submillimetre: galaxies, ISM, Cirrus, galaxies: evolution, Astrophysics - Cosmology and Nongalactic Astrophysics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), DATA RELEASE, Phase (waves), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, LUMINOSITY FUNCTIONS, Latitude, symbols.namesake, Settore FIS/05 - Astronomia e Astrofisica, Atlas (anatomy), medicine, Angular resolution, Planck, Early release, evolution [galaxies], Astrophysics::Galaxy Astrophysics, Science & Technology, STRONGLY LENSED GALAXIES, Astronomy and Astrophysics, Catalogues, galaxies: general, Galaxy, SPITZER, 0201 Astronomical And Space Sciences, Physics and Astronomy, Space and Planetary Science, CLUSTERS, catalogs, general [galaxies]
Abstract: We present the results of a cross-correlation of the Planck Early Release Compact Source catalogue (ERCSC) with the catalogue of Herschel-ATLAS sources detected in the phase 1 fields, covering 134.55 deg2. There are 28ERCSC sources detected by Planck at 857GHz in this area. Asmany as16 of them are probably high Galactic latitude cirrus; 10additional sources can be clearly identified as bright, low-z galaxies; one further source is resolved by Herschel as two relatively bright sources; and the last is resolved into an unusual condensation of low-flux, probably high-redshift point sources, around a strongly lensed Herschel-ATLAS source at z=3.26. Our results demonstrate that the higher sensitivity and higher angular resolution H-ATLAS maps provide essential information for the interpretation of candidate sources extracted from Planck sub-mm maps. © 2012 ESO., D.H. and M.L.C. acknowledge partial financial support from the Spanish Ministerio de Ciencia e Innovación project AYA2010-21766-C03-01 and the Consolider Ingenio- 2010 Programme project CSD2010-00064. D.H. also acknowledges the Spanish Ministerio de Educación for a José Castillejo’ mobility grant with reference JC2010-0096 and the Astronomy Department at the Cavendish Laboratory for their hospitality during the elaboration of this paper. The Italian group has been supported in part by ASI/INAF agreement No. I/009/10/0 and by INAF through the PRIN 2009 “New light on the early Universe with sub-mm spectroscopy”. F.J.C. acknowledges partial financial support from the Spanish Ministerio de Ciencia e Innovación project AYA2010-21490-C02-01.
Published: 2013

18. DISCOVERY OF AN ACTIVE GALACTIC NUCLEUS DRIVEN MOLECULAR OUTFLOW IN THE LOCAL EARLY-TYPE GALAXY NGC 1266

Author: Timothy A. Davis, Anne-Marie Weijmans, Leo Blitz, Sadegh Khochfar, K. Shapiro, Frédéric Bournaud, Nicholas Scott, Lisa M. Young, Davor Krajnović, Richard M. McDermid, Katherine Alatalo, Pierre Yves Lablanche, Jesus Falcon-Barosso, Laura A. Lopez, Maxime Bois, Pierre-Alain Duc, Eric Emsellem, Roger L. Davies, Paolo Serra, Harald Kuntschner, Tom Oosterloo, Raffaella Morganti, Thorsten Naab, Alison F. Crocker, Martin Bureau, Marc Sarzi, Sergio Martín, P. T. de Zeeuw, Michele Cappellari, Department of Astronomy, University of California, Physics Department, New Mexico Tech, Socorro, Sub-department of Astrophysics, Department of Physics, University of Oxford, Denys Wilkinson Building, Keble Road, Department of Astronomy and Astrophysics, University of California, Aerospace Research Laboratories, Northrop Grumman Aerospace Systems, Department of Astronomy, University of Massachusetts, European Southern Observatory, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), European Southern Observatory (ESO), Instituto de Astrofísica de Canarias (IAC), Max-Planck-Institut für Extraterrestriche Physik (MPE), Gemini Observatory, Netherlands Institute for Radio Astronomy (ASTRON), Max-Planck-Institut für Astrophysik (MPA), University of Hertfordshire [Hatfield] (UH), Dunlap Institute for Astronomy and Astrophysics, University of Toronto, and Astronomy
Subjects: Angular momentum, Active galactic nucleus, Milky Way, Astrophysics::High Energy Astrophysical Phenomena, RADIO GALAXIES, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, ELLIPTIC GALAXIES, 0103 physical sciences, STAR-FORMING GALAXIES, Astrophysics::Solar and Stellar Astrophysics, NEARBY GALAXIES, IC 5063, BLACK-HOLES, 010303 astronomy & astrophysics, galaxies: kinematics and dynamics, Astrophysics::Galaxy Astrophysics, Physics, Field galaxy, 010308 nuclear & particles physics, Star formation, Molecular cloud, Astronomy and Astrophysics, SAURON PROJECT, Galaxy, SPITZER, ISM: jets and outflows, GAS, Space and Planetary Science, MULTI-GAUSSIAN EXPANSION, Outflow, Astrophysics::Earth and Planetary Astrophysics, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], galaxies: ISM
Abstract: International audience; We report the discovery of a powerful molecular wind from the nucleus of the non-interacting nearby S0 field galaxy NGC 1266. The single-dish CO profile exhibits emission to ±400 km s-1 and requires a nested Gaussian fit to be properly described. Interferometric observations reveal a massive, centrally concentrated molecular component with a mass of 1.1 × 109 M sun and a molecular outflow with a molecular mass of ≈2.4 × 107 M sun. The molecular gas close to the systemic velocity consists of a rotating, compact nucleus with a mass of about 4.1 × 108 M sun within a radius of ≈60 pc. This compact molecular nucleus has a surface density of ≈2.7 × 104 M sun pc-2, more than two orders of magnitude larger than that of giant molecular clouds in the disk of the Milky Way, and it appears to sit on the Kennicutt-Schmidt relation despite its extreme kinematics and energetic activity. We interpret this nucleus as a disk that confines the outflowing wind. A mass outflow rate of ≈13 M sun yr-1 leads to a depletion timescale of lsim85 Myr. The star formation in NGC 1266 is insufficient to drive the outflow, and thus it is likely driven by the active galactic nucleus. The concentration of the majority of the molecular gas in the central 100 pc requires an extraordinary loss of angular momentum, but no obvious companion or interacting galaxy is present to enable the transfer. NGC 1266 is the first known outflowing molecular system that does not show any evidence of a recent interaction.
Published: 2011
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19. Herschel-ATLAS: Extragalactic number counts from 250 to 500 microns

Author: Rob Ivison, A. Verma, G. Lagache, Maarten Baes, Dave Frayer, E. E. Rigby, M. Pohlen, M. López-Caniego, Enzo Pascale, Antonio Cava, David Bonfield, A. Amblard, Loretta Dunne, Simon Dye, A. Dariush, Pasquale Temi, S. Buttiglione, P. van der Werf, Jacopo Fritz, Asantha Cooray, Lerothodi Leonard Leeuw, Chris Pearson, Robbie Richard Auld, Angela M. J. Mortier, D. Herranz, Saumyadip Samui, Jonathan P. Gardner, D. J. B. Smith, D. L. Clements, Matt J. Jarvis, Denis Burgarella, Maggie A. Thompson, S. J. Maddox, Steve Serjeant, M. Negrello, J. González-Nuevo, E. Ibar, Douglas Scott, I. Valtchanov, B. Sibthorpe, G. Rodighiero, G. de Zotti, Steve Eales, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Universidad de Cantabria, and Science and Technology Facilities Council (STFC)
Subjects: statistics [galaxies], UNIVERSE, galaxies [submillimeter], Astrophysics, Submilimeter: galaxies, 01 natural sciences, galaxies [Infrared], MAPS, 010303 astronomy & astrophysics, QB, media_common, Physics, education.field_of_study, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Atlas (topology), Galaxies: evolution, Wavelength, Physical Sciences, astro-ph.CO, statistics [Galaxy], Galaxies: statistics, Infrared: galaxies, Submillimeter: galaxies, Astronomy and Astrophysics, Space and Planetary Science, Astrophysics - Cosmology and Nongalactic Astrophysics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, Population, PREDICTIONS, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, STAR-FORMATION, Submillimetre: galaxies, Galaxy: statistics, 0103 physical sciences, Galaxy formation and evolution, 14. Life underwater, FIELD, education, Astrophysics::Galaxy Astrophysics, SURVEY SHADES, galaxies [Submilimeter], Science & Technology, SUBMILLIMETER GALAXIES, 010308 nuclear & particles physics, evolution [Galaxies], EVOLUTION, Redshift, Galaxy, MODEL, SPITZER, 0201 Astronomical And Space Sciences, Physics and Astronomy, Sky, Extraction methods
Abstract: 4 páginas, 1 figura, 1 tabla.-- Letter to the editor.-- Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.-- et al., [Aims]: The Herschel-ATLAS survey (H-ATLAS) will be the largest area survey to be undertaken by the Herschel Space Observatory. It will cover 550 sq. deg. of extragalactic sky at wavelengths of 100, 160, 250, 350 and 500 μm when completed, reaching flux limits (5σ) from 32 to 145 mJy. We here present galaxy number counts obtained for SPIRE observations of the first ∼14 sq. deg. observed at 250, 350 and 500 μm. [Methods]: Number counts are a fundamental tool in constraining models of galaxy evolution. We use source catalogs extracted from the H-ATLAS maps as the basis for such an analysis. Correction factors for completeness and flux boosting are derived by applying our extraction method to model catalogs and then applied to the raw observational counts. [Results]: We find a steep rise in the number counts at flux levels of 100−200 mJy in all three SPIRE bands, consistent with results from BLAST. The counts are compared to a range of galaxy evolution models. None of the current models is an ideal fit to the data but all ascribe the steep rise to a population of luminous, rapidly evolving dusty galaxies at moderate to high redshift.
Published: 2010
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20. FIR colours and SEDs of nearby galaxies observed with Herschel

Author: Stefano Zibetti, Matthew Joseph Griffin, Diane Cormier, Werner W. Zeilinger, Maud Galametz, L. Spinoglio, E. E. Rigby, Thomas M. Hughes, Andreas Papageorgiou, Aliakbar Dariush, Simone Bianchi, Jonathan Ivor Davies, Dario Fadda, Michael Pohlen, Anthony P. Jones, Marc Sauvage, Leslie K. Hunt, N. Lu, N. Castro-Rodriguez, Daniele Pierini, Gillian S. Wright, Jamie Stevens, Sacha Hony, Laure Ciesla, Herve Wozniak, Eli Dwek, Pierre Chanial, Jacopo Fritz, Kate Gudrun Isaak, Asantha Cooray, Ismael Perez-Fournon, L. Vigroux, Maximilien R. P. Schirm, Jason Glenn, Matthew Smith, D. J. Bomans, George J. Bendo, Alessandro Boselli, Marco Grossi, D. A. Garcia-Appadoo, Mattia Vaccari, M. Bradford, A. Rykala, Suzanne C. Madden, V. Buat, Koryo Okumura, Catherine Vlahakis, S. Sabatini, Christine D. Wilson, B. O'Halloran, Edvige Corbelli, James J. Bock, Frédéric Galliano, L. R. Levenson, Giuseppe Gavazzi, Markos Trichas, Helene Roussel, David L. Clements, Luca Cortese, Marcel Clemens, Benjamin L. Schulz, Seb Oliver, Stephane Charlot, Carlo Giovanardi, Maarten Baes, Emmanuel M. Xilouris, Joris Verstappen, Naseem Rangwala, Stephen Anthony Eales, N. Sacchi, P. Panuzzo, Robbie Richard Auld, T. J. Parkin, S. Sundar, M. J. Page, David Elbaz, M. Symeonidis, S. di Serego Alighieri, Haley Louise Gomez, Walter Kieran Gear, I. De Looze, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Science and Technology Facilities Council (STFC), Boselli, A, Ciesla, L, Buat, V, Cortese, L, Auld, R, Baes, M, Bendo, G, Bianchi, S, Bock, J, Bomans, D, Bradford, M, Castro Rodriguez, N, Chanial, P, Charlot, S, Clemens, M, Clements, D, Corbelli, E, Cooray, A, Cormier, D, Dariush, A, Davies, J, De Looze, I, di Serego Alighieri, S, Dwek, E, Eales, S, Elbaz, D, Fadda, D, Fritz, J, Galametz, M, Galliano, F, Garcia Appadoo, D, Gavazzi, G, Gear, W, Giovanardi, C, Glenn, J, Gomez, H, Griffin, M, Grossi, M, Hony, S, Hughes, T, Hunt, L, Isaak, K, Jones, A, Levenson, L, Lu, N, Madden, S, O'Halloran, B, Okumura, K, Oliver, S, Page, M, Panuzzo, P, Papageorgiou, A, Parkin, T, Perez Fournon, I, Pierini, D, Pohlen, M, Rangwala, N, Rigby, E, Roussel, H, Rykala, A, Sabatini, S, Sacchi, N, Sauvage, M, Schulz, B, Schirm, M, Smith, M, Spinoglio, L, Stevens, J, Sundar, S, Symeonidis, M, Trichas, M, Vaccari, M, Verstappen, J, Vigroux, L, Vlahakis, C, Wilson, C, Wozniak, H, Wright, G, Xilouris, E, Zeilinger, W, and Zibetti, S
Subjects: Infrared, Radio galaxy, DUST, Astrophysics, 01 natural sciences, galaxies [infrared], Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, QB, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], ATLAS, VIRGO CLUSTER, spiral [galaxies], Physical Sciences, astro-ph.CO, Astrophysics::Earth and Planetary Astrophysics, galaxies: ISM, Astrophysics - Cosmology and Nongalactic Astrophysics, galaxies: spiral, Active galactic nucleus, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Metallicity, INFRARED-EMISSION, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, Color temperature, infrared: galaxies, cD, FIS/05 - ASTRONOMIA E ASTROFISICA, 0103 physical sciences, Emissivity, STAR-FORMING GALAXIES, DISTRIBUTIONS, Astrophysics::Galaxy Astrophysics, Science & Technology, ISM [galaxies], 010308 nuclear & particles physics, Star formation, Astronomy and Astrophysics, Galaxy, UV, 0201 Astronomical And Space Sciences, SPITZER, SPECTRAL ENERGY-DISTRIBUTION, Physics and Astronomy, 13. Climate action, Space and Planetary Science, galaxies: elliptical and lenticular, cD, elliptical and lenticular [galaxies]
Abstract: We present infrared colours (in the 25-500 mic spectral range) and UV to radio continuum spectral energy distributions of a sample of 51 nearby galaxies observed with SPIRE on Herschel. The observed sample includes all morphological classes, from quiescent ellipticals to active starbursts. Active galaxies have warmer colour temperatures than normal spirals. In ellipticals hosting a radio galaxy, the far-infrared (FIR) emission is dominated bynthe synchrotron nuclear emission. The colour temperature of the cold dust is higher in quiescent E-S0a than in star-forming systems probably because of the different nature of their dust heating sources (evolved stellar populations, X-ray, fast electrons) and dust grain properties. In contrast to the colour temperature of the warm dust, the f350/f500 index sensitive to the cold dust decreases with star formation and increases with metallicity, suggesting an overabundance of cold dust or an emissivity parameter beta, Accepted for publication on A&A, Herschel special issue
Published: 2010
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21. Enhanced dust heating in the bulges of early-type spiral galaxies

Author: C. W. Engelbracht, L. K. Hunt, R. A. Skibba, J. L. Hinz, D. Calzetti, K. D. Gordon, H. Roussel, A. F. Crocker, K. A. Misselt, A. D. Bolatto, R. C. Kennicutt, P. N. Appleton, L. Armus, P. Beirão, B. R. Brandl, K. V. Croxall, D. A. Dale, B. T. Draine, G. Dumas, A. Gil de Paz, B. Groves, C.-N. Hao, B. D. Johnson, J. Koda, O. Krause, A. K. Leroy, S. E. Meidt, E. J. Murphy, N. Rahman, H.-W. Rix, K. M. Sandstrom, M. Sauvage, E. Schinnerer, J.-D. T. Smith, S. Srinivasan, L. Vigroux, F. Walter, B. E. Warren, C. D. Wilson, M. G. Wolfire, and S. Zibetti
Subjects: Astrofísica, Cosmology and Nongalactic Astrophysics (astro-ph.CO), INFRARED-EMISSION, MU-M, galaxies [submillimeter], FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, galaxies [infrared], STAR-FORMATION, Bulge, Astrophysics::Solar and Stellar Astrophysics, NEARBY GALAXIES, COLD DUST, Stellar density, Astrophysics::Galaxy Astrophysics, Physics, Spiral galaxy, ISM [galaxies], extinction, Astronomy and Astrophysics, DISK GALAXIES, Galaxy, Early type, Astronomía, Temperature gradient, Wavelength, SPITZER, SPECTRAL ENERGY-DISTRIBUTION, Physics and Astronomy, Space and Planetary Science, MULTIBAND IMAGING PHOTOMETER, dust, Astrophysics::Earth and Planetary Astrophysics, ABSOLUTE CALIBRATION, Bar (unit), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Stellar density and bar strength should affect the temperatures of the cool (T ~ 20-30 K) dust component in the inner regions of galaxies, which implies that the ratio of temperatures in the circumnuclear regions to the disk should depend on Hubble type. We investigate the differences between cool dust temperatures in the central 3 kpc and disk of 13 nearby galaxies by fitting models to measurements between 70 and 500 microns. We attempt to quantify temperature trends in nearby disk galaxies, with archival data from Spitzer/MIPS and new observations with Herschel/SPIRE, which were acquired during the first phases of the Herschel observations for the KINGFISH (key insights in nearby galaxies: a far-infrared survey with Herschel) sample. We fit single-temperature modified blackbodies to far-infrared and submillimeter measurements of the central and disk regions of galaxies to determine the temperature of the component(s) emitting at those wavelengths. We present the ratio of central-region-to-disk-temperatures of the cool dust component of 13 nearby galaxies as a function of morphological type. We find a significant temperature gradient in the cool dust component in all galaxies, with a mean center-to-disk temperature ratio of 1.15 +/- 0.03. The cool dust temperatures in the central ~3 kpc of nearby galaxies are 23(+/-3)% hotter for morphological types earlier than Sc, and only 9(+/-3)% hotter for later types. The temperature ratio is also correlated with bar strength, with only strongly barred galaxies having a ratio over 1.2. The strong radiation field in the high stellar density of a galactic bulge tends to heat the cool dust component to higher temperatures, at least in early-type spirals with relatively large bulges, especially when paired with a strong bar., Comment: Accepted for publication on the A&A Herschel Special Issue
Published: 2010

22. 100 μm and 160 μm emission as resolved star-formation rate estimators in M 33 (HERM33ES)

Author: E. M. Xilouris, F. F. S. van der Tak, B. S. Koribalski, Fatemeh Tabatabaei, J. Braine, Frank P. Israel, S. Verley, Francoise Combes, Markus Röllig, D. Calzetti, P. van der Werf, M. Boquien, C. Kramer, G. Quintana-Lacaci, Monica Relaño, Remo P. J. Tilanus, S. D. Lord, Gordon J. Stacey, Christof Buchbender, Frank Bertoldi, Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Department of Astronomy, University of Massachusetts System (UMASS), Instituto de RadioAstronomía Milimétrica (IRAM), Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Radioastronomie (MPIFR), Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB), Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Leiden Observatory [Leiden], Universiteit Leiden, Australia Telescope National Facility, Australian National University (ANU), Dpto. Fisica Teorica y del Cosmos, Universidad de Granada = University of Granada (UGR), Dept. fısica Teorica y del Cosmos, Astronomy, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1, École normale supérieure - Paris (ENS Paris)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), Universiteit Leiden [Leiden], Universidad de Granada (UGR), and École normale supérieure - Paris (ENS Paris)
Subjects: galaxies: spiral, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Infrared, ULTRAVIOLET, FOS: Physical sciences, Scale (descriptive set theory), DUST, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Luminosity, infrared: galaxies, 0103 physical sciences, PHOTOMETRY, Astrophysics::Solar and Stellar Astrophysics, TOTAL INFRARED LUMINOSITY, NEARBY GALAXIES, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, CALIBRATION, FORMING GALAXIES, 010308 nuclear & particles physics, Star formation, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Estimator, Sigma, Astronomy and Astrophysics, galaxies: individual: M33, Cosmology and Extragalactic Astrophysics, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Astrophysics - Astrophysics of Galaxies, Galaxy, SPITZER, EXTINCTION, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), galaxies: star formation, Astrophysics::Earth and Planetary Astrophysics, FORMATION RATE INDICATORS, Astrophysics - Cosmology and Nongalactic Astrophysics, Galaxy Astrophysics
Abstract: Over the past few years several studies have provided estimates of the SFR (star-formation rate) or the total infrared luminosity from just one infrared band. However these relations are generally derived for entire galaxies, which are known to contain a large scale diffuse emission that is not necessarily related to the latest star-formation episode. We provide new relations to estimate the SFR from resolved star-forming regions at 100 mum and 160 mum. We select individual star-forming regions in the nearby (840 kpc) galaxy M33. We estimate the SFR combining the emission in Halpha and at 24 mum to calibrate the emission at 100 mum and 160 mum as SFR estimators, as mapped with PACS/Herschel. The data are obtained in the framework of the HERM33ES open time key project. There is less emission in the HII regions at 160 mum than at 100 mum. Over a dynamic range of almost 2 dex in Sigma(SFR) we find that the 100 mum emission is a nearly linear estimator of the SFR, whereas that at 160 mum is slightly superlinear. The behaviour of individual star-forming regions is surprisingly similar to that of entire galaxies. At high Sigma(SFR), star formation drives the dust temperature, whereas uncertainties and variations in radiation-transfer and dust-heated processes dominate at low Sigma(SFR). Detailed modelling of both galaxies and individual star forming regions will be needed to interpret similarities and differences between the two and assess the fraction of diffuse emission in galaxies., 5 pages, 3 figures, accepted for publication in the A&A Herschel special issue
Published: 2010
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23. Herschel-ATLAS: Evolution of the 250 μm luminosity function out to z = 0.5

Author: M. N. Bremer, Aaron S. G. Robotham, L. Leeuw, Ewan Cameron, Steve Eales, Richard J. Tuffs, G. Lagache, J. González-Nuevo, Andrew M. Hopkins, Denis Hill, Maggie A. Thompson, B. Sibthorpe, D. H. P. Jones, Antonio Cava, Haley Louise Gomez, A. Verma, D. J. B. Smith, L. Kelvin, David Bonfield, Simon Dye, Jacopo Fritz, James Dunlop, Asantha Cooray, D. L. Clements, R. G. Sharp, S. Buttiglione, Pasquale Temi, Andrew Blain, S. J. Maddox, Matthew Prescott, D. Herranz, Denis Burgarella, Saumyadip Samui, M. J. Page, I. Valtchanov, Maarten Baes, Michał J. Michałowski, Peder Norberg, H. Parkinson, D. Rigopoulou, Jon Loveday, G. Rodighiero, Steven P. Bamford, Simon P. Driver, M. Pohlen, G. de Zotti, Enzo Pascale, Steve Serjeant, A. Dariush, E. E. Rigby, E. van Kampen, Matt J. Jarvis, P. van der Werf, Douglas Scott, Jonathan P. Gardner, Cristina Popescu, M. Negrello, Ivan K. Baldry, Rob Ivison, Loretta Dunne, John A. Peacock, Robbie Richard Auld, Jochen Liske, M. López-Caniego, David T. Frayer, E. Ibar, Scott M. Croom, A. Amblard, Universidad de Cantabria, and Science and Technology Facilities Council (STFC)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), luminosity function, mass function [Galaxies], Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Cosmology: observations, Galaxies: luminosity function, mass function, Large-scale structure of Universe, Astronomy and Astrophysics, Space and Planetary Science, Astronomy & Astrophysics, Luminosity, STAR-FORMATION, Atlas (anatomy), Galaxies: luminosity function, medicine, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Galaxy Astrophysics, Luminosity function (astronomy), QB, luminosity function [galaxies], Physics, REDSHIFT SURVEY, Science & Technology, RADIO, SUBMILLIMETER LUMINOSITY, IDENTIFICATION, COUNTERPARTS, Galaxy, Redshift, observations [cosmology], GALAXIES, SPITZER, 0201 Astronomical And Space Sciences, medicine.anatomical_structure, Physics and Astronomy, mass function, Mass function, Physical Sciences, astro-ph.CO, Llarge-scale structure of Universe, DEEP-FIELD-SOUTH, large-scale structure of Universe, SKY SURVEY, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: 5 páginas, 4 figuras.-- Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.-- et al., We have determined the luminosity function of 250 μm-selected galaxies detected in the ~14 deg2 science demonstration region of the Herschel-ATLAS project out to a redshift of z = 0.5. Our findings very clearly show that the luminosity function evolves steadily out to this redshift. By selecting a sub-group of sources within a fixed luminosity interval where incompleteness effects are minimal, we have measured a smooth increase in the comoving 250 μm luminosity density out to z = 0.2 where it is 3.6+1.4-0.9 times higher than the local value., S.D. Acknowledges the UK STFC for support.
Published: 2010

24. The space infrared telescope for cosmology and astrophysics: SPICA A joint mission between JAXA and ESA

Author: SWINYARD, Bruce, NAKAGAWA, Takao, MERKEN, Patrick, ROYER, Pierre, SOUVERIJNS, Tim, VANDENBUSSCHE, Bart, WAELKENS, Christoffel, DAVIS, Peter, DI FRANCESCO, James, HALPERN, Mark, HOUDE, Martin, JOHNSTONE, Doug, JONCAS, Gilles, NAYLOR, David, PLUME, Rene, SCOTT, Douglas, ABERGEL, A., BENSAMMAR, S., BRAINE, J., BUAT, V., BURGARELLA, D., CAIS, Ph., DOLE, H., DUBAND, L., ELBAZ, D., GERIN, M., GIARD, M., GOICOECHEA, J., JOBLIN, C., JONES, A., KNEIB, J. P., LAGACHE, Guilaine, MADDEN, S., PONS, R., PAJOT, F., RAMBAUD, D., RAVERA, L., RISTORCELLI, I., RODRIGUEZ, L., VIVES, S., ZAVAGNO, Annie, GEIS, Norbert, KRAUSE, Oliver, LUTZ, Dieter, POGLITSCH, Albrecht, RAAB, Walfried, STEGMAIER, Jutta, STURM, Eckhard, TUFFS, Richard, LEE, Hyung Mok, KOO, Bon-Chul, IM, Myungshin, PAK, Soojong, HAN, Wonyong, PARK, Jang-Hyun, NAM, Uk-Won, JIN, Ho, LEE, Dae-Hee, YUK, In-Soo, LEE, Sungho, AIKAWA, Yuri, ARIMOTO, Nobuo, DOI, Yasuo, ENYA, Keigo, FUKAGAWA, Misato, FURUSHO, Reiko, HASEGAWA, Sunao, HAYASHI, Masahiko, HONDA KANAGAWA, Mitsuhiko, IDA, Shigeru, IMANISHI, MASATOSHI, INUTSUKA, Shu-Ichiro, IZUMIURA, Hideyuki, KAMAYA, Hideyuki, KANEDA, Hidehiro, KASUGA, Toshihiro, KATAZA, Hirokazu, KAWABATA, Koji, KAWADA, Mitsunobu, KAWAKITA, Hideyo, KII, Tsuneo, KODA, Jin, KODAMA, Tadayuki, KOKUBO, Eiichiro, KOMATSU, Keiji, MATSUHARA, Hideo, MATSUMOTO, Toshio, MATSUURA, Shuji, MIYATA, Takashi, MIYATA, Murakam, NAGATA, Hirohisa, NAGATA, Tetsuya, NAKAJIMA, Tadashi, NAOTO, Kobayashi, NISHI, Ryoichi, NODA, Atsushi, OKAMOTO, Atsushi, OKAMOTO, Yoshiko K., OMUKAI, Kazuyuki, ONAKA, Takashi, OOTSUBO, Takafumi, OUCHI, Masami, SAITO, Hirobumi, SATO, Yoichi, SAKO, Shigeyuki, SEKIGUCHI, Tomohiko, SHIBAI, Hiroshi, SUGITA, Hiroyuki, SUGITANI, Koji, SUSA, Hajime, PYO, Tae-Soo, TAMURA, Motohide, UEDA, Yoshihiro, UENO, Munetaka, WADA, Takehiko, WATANABE, Jun'Ichi, YAMADA, Toru, YAMAMURA, Issei, YOSHIDA, Naoki, YOSHIMI, Kitamura, YUI, Yukari, BENEDETTINI, Milena, CERULLI, Riccardo, DI GIORGIO, Anna, MOLINARI, Sergio, ORFEI, Renato, PEZZUTO, Stefano, PIAZZO, Lorenzo, SARACENO, Paolo, SPINOGLIO, Luigi, DE GRAAUW, Thijs, DE KORTE, Piet, HELMICH, Frank, HOEVERS, Henk, HUISMAN, Robert, SHIPMAN, Russell, VAN DER TAK, Floris, VAN DER WERF, Paul, WILD, Wolfgang, ACOSTA-PULIDO, Jose, CERNICHARO, Jose, HERREROS, Jose, MARTIN-PINTADO, Jesus, NAJARRO, Francisco, PEREZ-FOURMON, Ismael, RAMON PARDO, Juan, GOMEZ, Francisca, CASTRO RODRIGUEZ, Nieves, ADE, Peter, BARLOW, Mike, CLEMENTS, David, FERLET, Marc, FRASER, Helen, GRIFFIN, Douglas, GRIFFIN, Matthew, HARGRAVE, Peter, ISAAK, Kate, IVISON, Robert, MANSOUR, Malik, LANIESSE, Jonathan, MAUSKOPF, Phillip, MOROZOV, Dmitry, OLIVER, Seb, ORLANDO, Angiola, PAGE, Mathew, POPESCU, Cristina, SERJEANT, Stephen, SUDIWALA, Rashmi, RIGOPOULOU, Dimitra, WALKER, Ian, WHITE, Glenn, VITI, Serena, WINTER, Berend, BOCK, Jamie, BRADFORD, Matt, HARWIT, Martin, HOLMES, Warren, Institut Méditerranéen d'Ecologie et de Paléoécologie (IMEP), Université Paul Cézanne - Aix-Marseille 3-Centre National de la Recherche Scientifique (CNRS)-Avignon Université (AU)-Université de Provence - Aix-Marseille 1, Institute of Atomic Physics, Université de Roumanie, Groundwater Tracing Unit, Department of Geological Sciences, School of Environmental Sciences [Norwich], University of East Anglia [Norwich] (UEA), Institut de Recherche en Immunologie et en Cancérologie [UdeM-Montréal] (IRIC), Université de Montréal (UdeM), Department of Zoology, University of Otago [Dunedin, Nouvelle-Zélande], Transplantation Biology Group, Imperial College London, 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), Observatoire de Paris - Site de Paris (OP), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - 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(Adobe Advanced Technology Labs), Adobe Systems Inc., Defence Evaluation and Research Agency (DERA), Ministry of Defence (UK) (MOD)-Propulsion and Performance Department, Centre for Air Transport and the Environment (CATE), Manchester Metropolitan University (MMU), Department of Chemistry, Williams Hall-Kent State University, School of Earth and Atmospheric Sciences [Atlanta], Georgia Institute of Technology [Atlanta], Department of Earth and Planetary Sciences [Kobe], Kobe University, National Institute of Agro-Environmental Sciences (NIAES), Department of Earth System Science and Technology [Fukuoka] (ESST), Kyushu University [Fukuoka], Tokyo Institute of Technology [Tokyo] (TITECH), Department of Information and Communication Engineering, Graduate School of Information Science and Technology-The University of Tokyo (UTokyo), Department of Physics and Earth Sciences, University of the Ryukyus [Okinawa], Japan Agency for Marine-Earth Science and Technology (JAMSTEC), Center for Climate System Research [Kashiwa] (CCSR), The University of Tokyo (UTokyo), School of Humanities [Univ of Toyama], University of Toyama, Department of Mechanical System (Hiroshima University), Hiroshima University, High Temperature Plasma Center [Tokyo], Discrete Optimization Laboratory, Toyohashi University of Technology, Hatakeyama Laboratory, University of Electro-Communications [Tokyo] (UEC)-Tohoku University [Sendai], Institute of Industrial Science (IIS), Institut de génétique et biologie moléculaire et cellulaire (IGBMC), Université Louis Pasteur - 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Paris (ENS Paris)-Centre National de la Recherche Scientifique (CNRS), Service de neurologie 1 [CHU Pitié-Salpétrière], Assistance publique - Hôpitaux de Paris (AP-HP) (APHP)-CHU Pitié-Salpêtrière [APHP], Stanford Linear Accelerator Center (SLAC), Astronomy, Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Météo-France -Institut de Recherche pour le Développement (IRD)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP), The University of Tokyo (UTokyo)-Graduate School of Information Science and Technology, Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-CHU Pitié-Salpêtrière [AP-HP], and Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Sorbonne Université (SU)-Sorbonne Université (SU)
Subjects: [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Infrared telescope, UNIVERSE, Astrophysics, Spica, Astrophysics::Cosmology and Extragalactic Astrophysics, POLYCYCLIC AROMATIC-HYDROCARBON, 7. Clean energy, 01 natural sciences, Space missions, Cosmology, Space exploration, law.invention, STAR-FORMATION, 010309 optics, Telescope, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Spitzer Space Telescope, law, 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, Infrared astronomy, SPECTRUM, Spacecraft, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], SUBMILLIMETER GALAXIES, business.industry, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, MODEL, SPITZER, PAHS, Space and Planetary Science, Infrared, Physics::Space Physics, IR, Astrophysics::Earth and Planetary Astrophysics, business, EMISSION
Abstract: International audience; The Space Infrared telescope for Cosmology and Astrophysics (SPICA) is planned to be the next space astronomy mission observing in the infrared. The mission is planned to be launched in 2017 and will feature a 3.5 m telescope cooled to 30 microns wavelength). We describe the scientific advances that will be made possible by this large increase in sensitivity and give details of the mission, spacecraft and focal plane conceptual design.
Published: 2009
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25. The origin of the infrared emission in radio galaxies I: new mid- to far-infrared and radio observations of the 2Jy sample

Author: Catherine L. Buchanan, D. Dicken, David Axon, Tom Oosterloo, Clive Tadhunter, R. Morganti, and Kapteyn Astronomical Institute
Subjects: Infrared, Radio galaxy, galaxies : active, Astrophysics::High Energy Astrophysical Phenomena, SCHEMES, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, POLARIMETRY, law.invention, Telescope, Far infrared, Spitzer Space Telescope, law, Astrophysics::Galaxy Astrophysics, Physics, POWERFUL, SPECTROSCOPY, infrared : galaxies, NUCLEI, Star formation, Astrophysics (astro-ph), Astronomy and Astrophysics, 3CR QUASARS, LOUD, Redshift, Galaxy, SPITZER, Space and Planetary Science, MULTIBAND IMAGING PHOTOMETER, ABSOLUTE CALIBRATION
Abstract: As part of a large study to investigate the nature of the longer wavelength continuum emission of radio-loud AGN, we present new mid to far-infrared (MFIR) and high frequency radio observations for a complete sample of 2Jy powerful, southern radio galaxies at intermediate redshifts (0.05, Comment: 23 pages, 8 figures, Accepted for publication in the Astrophysical Journal
Published: 2008

26. Recent star formation in the Lupus clouds as seen byHerschel

Author: Sergio Molinari, J. P. Bernard, D. Polychroni, Nick L. J. Cox, A. Facchini, Martin Hennemann, A. Di Giorgio, Stefano Pezzuto, Davide Elia, Nicola Schneider, E. Schisano, Kazi L.J. Rygl, Tracey Hill, Cassandra Fallscheer, L. Spinoglio, M. R. Pestalozzi, Glenn J. White, Ph. André, Frédérique Motte, Derek Ward-Thompson, Quang Nguyen-Luong, J. Di Francesco, Vincent Minier, Sylvain Bontemps, Milena Benedettini, Nicolas Peretto, Leonardo Testi, S. Sadavoy, Vera Könyves, Laboratoire d'Astrophysique de Grenoble (LAOG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Istituto di Fisica dello Spazio Interplanetario (IFSI), Consiglio Nazionale delle Ricerche (CNR), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Engineering Department, University of Cambridge [UK] (CAM), FORMATION STELLAIRE 2013, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB), Herzberg Institute of Astrophysics, National Research Council of Canada (NRC), foreign laboratories (FL), CERN [Genève], Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Antarctic Research a European Network for Astrophysics (ARENA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), European Southern Observatory (ESO), School of Physics and Astronomy [Cardiff], Cardiff University, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG ), Observatoire des Sciences de l'Univers de Grenoble (OSUG), Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), and Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB)
Subjects: endocrine system, Spitzer, Stars: formation, Young stellar object, Extinction (astronomy), Lupus (constellation), FOS: Physical sciences, Gould belt, Astrophysics, Surveys, 01 natural sciences, Stars: protostars, ISM: individual objects, 0103 physical sciences, Star formation rates, 010303 astronomy & astrophysics, Infrared: ISM, Physics, HERSCHEL, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], 010308 nuclear & particles physics, Star formation, Star formations, Pre-main sequences, Astronomy and Astrophysics, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Stars, Astrophysics - Astrophysics of Galaxies, Young stellar objects, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA)
Abstract: We present a study of the star formation histories of the Lupus I, III, and IV clouds using the Herschel 70-500 micron maps obtained by the Herschel Gould Belt Survey Key Project. By combining the new Herschel data with the existing Spitzer catalog we obtained an unprecedented census of prestellar sources and young stellar objects in the Lupus clouds, which allowed us to study the overall star formation rate (SFR) and efficiency (SFE). The high SFE of Lupus III, its decreasing SFR, and its large number of pre-main sequence stars with respect to proto- and prestellar sources, suggest that Lupus III is the most evolved cloud, and after having experienced a major star formation event in the past, is now approaching the end of its current star-forming cycle. Lupus I is currently undergoing a large star formation event, apparent by the increasing SFR, the large number of prestellar objects with respect to more evolved objects, and the high percentage of material at high extinction (e.g., above A_V=8 mag). Also Lupus IV has an increasing SFR; however, the relative number of prestellar sources is much lower, suggesting that its star formation has not yet reached its peak., Comment: 9 pages, 5 figures, accepted for publication in Astronomy and Astrophysics
Published: 2012
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27. TheHerschelVirgo Cluster Survey

Author: George J. Bendo, Stefano Zibetti, T. M. Hughes, Catherine Vlahakis, S. Sabatini, Edvige Corbelli, Matthew Smith, Aliakbar Dariush, Jacopo Fritz, Maarten Baes, Carlo Giovanardi, Luca Cortese, D. J. Bomans, Daniele Pierini, S. di Serego Alighieri, Marco Grossi, Jonathan Ivor Davies, Anthony P. Jones, Joris Verstappen, Emmanuel M. Xilouris, Suzanne C. Madden, Simone Bianchi, I. De Looze, Dario Fadda, Michael Pohlen, Leslie K. Hunt, Alessandro Boselli, Giuseppe Gavazzi, D. A. Garcia-Appadoo, and Marcel Clemens
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), dwarf [galaxies], NGC 205, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, RADIATIVE-TRANSFER, Cluster (physics), Astrophysics::Solar and Stellar Astrophysics, COLD DUST, Astrophysics::Galaxy Astrophysics, Cosmic dust, Dwarf galaxy, Physics, ISM [galaxies], extinction, ORIGIN, individual: VCC951 [galaxies], Astronomy and Astrophysics, individual: VCC781 [galaxies], CATALOG, Virgo Cluster, EVOLUTION, SIMULATIONS, Galaxy, Ram pressure, MODEL, SPITZER, Spire, Physics and Astronomy, Space and Planetary Science, Elliptical galaxy, DIGITAL SKY SURVEY, dust, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We use the Science Demonstration Phase data of the Herschel Virgo Cluster Survey to search for dust emission of early-type dwarf galaxies in the central regions of the Virgo Cluster as an alternative way of identifying the interstellar medium.We present the first possible far-infrared detection of cluster early-type dwarf galaxies: VCC781 and VCC951 are detected at the 10 sigma level in the SPIRE 250 micron image. Both detected galaxies have dust masses of the order of 10^5 Msun and average dust temperatures ~20K. The detection rate (less than 1%) is quite high compared to the 1.7% detection rate for Hi emission, considering that dwarfs in the central regions are more Hi deficient. We conclude that the removal of interstellar dust from dwarf galaxies resulting from ram pressure stripping, harassment, or tidal effects must be as efficient as the removal of interstellar gas., Letter accepted for publication in A&A (Herschel special issue)
Published: 2010
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28. TheHerschelSpace Observatory view of dust in M81

Author: Marc Sauvage, N. Lu, Pierre Chanial, Walter Kieran Gear, L. Vigroux, Pasquale Panuzzo, M. Symeonidis, Herve Wozniak, Diane Cormier, George J. Bendo, B. O'Halloran, James J. Bock, M. J. Barlow, Werner W. Zeilinger, Jamie Stevens, Mattia Vaccari, E. E. Rigby, Stephane Charlot, Helene Roussel, David L. Clements, Luca Cortese, Naseem Rangwala, T. J. Parkin, Michael Pohlen, N. Castro-Rodriguez, Matthew Joseph Griffin, Matthew Smith, Sacha Hony, S. Sundar, Maud Galametz, Alessandro Boselli, A. Cooray, Gillian S. Wright, Christine D. Wilson, M. Bradford, Haley Louise Gomez, Stephen Anthony Eales, Koryo Okumura, Andreas Papageorgiou, Eli Dwek, Maximilien R. P. Schirm, Laure Ciesla, Kate Gudrun Isaak, Maarten Baes, N. Sacchi, Suzanne C. Madden, L. R. Levenson, Benjamin L. Schulz, Markos Trichas, Seb Oliver, V. Buat, Ismael Perez-Fournon, Mat Page, Jason Glenn, Robbie Richard Auld, D. Elbaz, Frédéric Galliano, L. Spinoglio, A. Rykala, Jonathan Ivor Davies, 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), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Observatoire astronomique de Strasbourg (ObAS), and Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: galaxies: spiral, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Active galactic nucleus, TELESCOPE, H-ALPHA, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, THINGS, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, STAR-FORMATION RATES, individual: M81 [galaxies], galaxies: individual: M81, Bulge, Astrophysics::Solar and Stellar Astrophysics, Surface brightness, FIELD, Astrophysics::Galaxy Astrophysics, QB, Physics, Spiral galaxy, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], ISM [galaxies], Spectral density, Astronomy and Astrophysics, Radius, Space observatory, GALAXIES, SPITZER, Stars, spiral [galaxies], Physics and Astronomy, [SDU]Sciences of the Universe [physics], Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, EMISSION, galaxies: ISM, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We use Herschel Space Observatory data to place observational constraints on the peak and Rayleigh-Jeans slope of dust emission observed at 70-500 microns in the nearby spiral galaxy M81. We find that the ratios of wave bands between 160 and 500 microns are primarily dependent on radius but that the ratio of 70 to 160 micron emission shows no clear dependence on surface brightness or radius. These results along with analyses of the spectral energy distributions imply that the 160-500 micron emission traces 15-30 K dust heated by evolved stars in the bulge and disc whereas the 70 micron emission includes dust heated by the active galactic nucleus and young stars in star forming regions., Accepted for A & A Herschel special issue
Published: 2010
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29. A search for debris disks in the Herschel -ATLAS

Author: Eduardo Gonzalez-Solares, Edo Ibar, Michael Pohlen, Lerothodi Leonard Leeuw, Saumyadip Samui, Matt J. Jarvis, Aprajita Verma, Guilaine Lagache, Jamie Stevens, M. López-Caniego, Jacopo Fritz, A. Amblard, Daniel J. Smith, J. Vieiria, Asantha Cooray, J. González-Nuevo, Loretta Dunne, Douglas Scott, Glenn J. White, P. Temi, S. Buttiglione, B. Sibthorpe, D. G. Bonfield, David T. Frayer, Jonathan P. Marshall, Denis Burgarella, Aliakbar Dariush, Antonio Cava, Maarten Baes, Mark Thompson, Rob Ivison, Mattia Negrello, Simon Dye, Ivan Valtchanov, Enzo Pascale, E. Vidal Perez, D. Herranz, Stephen Serjeant, Robbie Richard Auld, Stephen Anthony Eales, E. E. Rigby, Steve Maddox, G. de Zotti, Giulia Rodighiero, David L. Clements, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Universidad de Cantabria, and Science and Technology Facilities Council (STFC)
Subjects: Philosophy and Religion, Submillimeter: stars, PHOTOMETRIC SYSTEM, Astrophysics, 01 natural sciences, Circumstellar matter, Submillimeter: planetary systems, Astronomy and Astrophysics, Space and Planetary Science, Mathematics::Group Theory, WIDE-FIELD CAMERA, SUBMILLIMETER IMAGES, 010303 astronomy & astrophysics, QB, Earth and Planetary Astrophysics (astro-ph.EP), education.field_of_study, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], medicine.anatomical_structure, Physical Sciences, astro-ph.CO, Geology, Astrophysics - Cosmology and Nongalactic Astrophysics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), astro-ph.GA, Likelihood ratio method, Population, FOS: Physical sciences, Astronomy & Astrophysics, circumstellar matter, COOL STARS, COLORS, Atlas (anatomy), 0103 physical sciences, medicine, education, Debris disk, Science & Technology, stars [submillimeter], 010308 nuclear & particles physics, planetary systems [submillimeter], Astrophysics - Astrophysics of Galaxies, Debris, Galaxy, EVOLUTION, 2MASS, 0201 Astronomical And Space Sciences, Stars, SPITZER, Astrophysics of Galaxies (astro-ph.GA), astro-ph.EP, DIGITAL SKY SURVEY, NEARBY STARS, Main sequence, Astrophysics - Earth and Planetary Astrophysics
Abstract: Thompson, M. A. et al., Aims. We aim to demonstrate that the Herschel-ATLAS (H-ATLAS) is suitable for a blind and unbiased survey for debris disks by identifying candidate debris disks associated with main sequence stars in the initial science demonstration field of the survey. We show that H-ATLAS reveals a population of far-infrared/sub-mm sources that are associated with stars or star-like objects on the SDSS main-sequence locus. We validate our approach by comparing the properties of the most likely candidate disks to those of the known population. Methods. We use a photometric selection technique to identify main sequence stars in the SDSS DR7 catalogue and a Bayesian Likelihood Ratio method to identify H-ATLAS catalogue sources associated with these main sequence stars. Following this photometric selection we apply distance cuts to identify the most likely candidate debris disks and rule out the presence of contaminating galaxies using UKIDSS LAS K-band images. Results. We identify 78 H-ATLAS sources associated with SDSS point sources on the main-sequence locus, of which two are the most likely debris disk candidates: H-ATLAS J090315.8 and H-ATLAS J090240.2. We show that they are plausible candidates by comparing their properties to the known population of debris disks. Our initial results indicate that bright debris disks are rare, with only 2 candidates identified in a search sample of 851 stars. We also show that H-ATLAS can derive useful upper limits for debris disks associated with Hipparcos stars in the field and outline the future prospects for our debris disk search programme. © 2010 ESO
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29 results on '"SPITZER"'

1. JWST MIRI/MRS in-flight absolute flux calibration and tailored fringe correction for unresolved sources

2. Precision measurement of a brown dwarf mass in a binary system in the microlensing event OGLE-2019-BLG-0033/MOA-2019-BLG-035

3. B-fields in Star-forming Region Observations (BISTRO): Magnetic Fields in the Filamentary Structures of Serpens Main

4. K2 and Spitzer phase curves of the rocky ultra-short-period planet K2-141 b hint at a tenuous rock vapor atmosphere

5. A First Look into the Nature of JWST/MIRI 7.7 μm Sources from SMACS 0723

6. GOODS-ALMA: Using IRAC and VLA to probe fainter millimeter galaxies

7. Have we seen all the galaxies that comprise the cosmic infrared background at 250 μm ≤ λ ≤ 500 μm?

8. Dust evolution across the Horsehead nebula

9. The dust content of the Crab Nebula

10. HFF-DeepSpace photometric catalogs of the 12 Hubble frontier fields, clusters, and parallels: photometry, photometric redshifts, and stellar masses

11. SPICA —A Large Cryogenic Infrared Space Telescope: Unveiling the Obscured Universe

12. De‐blending deep Herschel surveys: A multi‐wavelength approach

13. Infrared Emission by Dust Around λ Bootis Stars

14. Cold galaxies

15. Extreme conditions in a close analog to the young solar system : Herschel observations of ε Eridani

16. WISE detections of known QSOs at redshifts greater than six

17. Herschel-ATLAS: Planck sources in the phase 1 fields

18. DISCOVERY OF AN ACTIVE GALACTIC NUCLEUS DRIVEN MOLECULAR OUTFLOW IN THE LOCAL EARLY-TYPE GALAXY NGC 1266

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

20. FIR colours and SEDs of nearby galaxies observed with Herschel

21. Enhanced dust heating in the bulges of early-type spiral galaxies

22. 100 μm and 160 μm emission as resolved star-formation rate estimators in M 33 (HERM33ES)

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

24. The space infrared telescope for cosmology and astrophysics: SPICA A joint mission between JAXA and ESA

25. The origin of the infrared emission in radio galaxies I: new mid- to far-infrared and radio observations of the 2Jy sample

26. Recent star formation in the Lupus clouds as seen byHerschel

27. TheHerschelVirgo Cluster Survey

28. TheHerschelSpace Observatory view of dust in M81

29. A search for debris disks in the Herschel -ATLAS

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