DOCSLIB.ORG

Dusty Universe

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text

Load more

Dusty Universe Asantha Cooray • Far-Infrared Background • Dusty galaxies and their role in galaxy formation and evolution • Far-IR spectroscopy as a probe of interstellar medium and AGN activity • Review of results from Herschel Space Observatory and ALMA Outline Asantha Cooray, UC Irvine Dusty Universe 2016 5 10 3 Microwaves 10 -1 sr Optical -2 1 10 X-ray UV -1 Infrared 10 Gamma-ray Intensity nW m -3 Radio 10 -5 10 -18 -16 -14 -12 -10 -8 -6 -4 -2 0 2 10 10 10 10 10 10 10 10 10 10 10 Wavelength (meters) Cosmic Background Light Asantha Cooray, UC Irvine Dusty Universe 2016 100 DIRBE CIBER -1 HST UVS/STIS IRAS sr -2 IRTS 10 Galaxy PACS nW m FIRAS counts SPIRE IRAC HESS ISO Intensity 1 MIPS SCUBA 0.1 1.0 10.0 100.0 Wavelength Cosmic Background Light Asantha Cooray, UC Irvine Dusty Universe 2016 Star Formation in the Rosette Nebula PACS 70 & 160 um + SPIRE 250 um 250µm 350µm 500µm 10 arcmin GOODS-N • FIRAS total background Source Counts 250, 350, 500 µm 15%, 10%, 6% • P(D) 250, 350, 500 µm 65%, 60%, 45% confusion confusion σ σ 5 5 • Stacking: 250, 350, 500 µm 80%, 80%, 85% Of course: The remainder are the most interesting sources! E.g. z > 3 galaxy populations Resolving the extragalactic background spectrum Asantha Cooray, UC Irvine Far-Infrared 2016 AAS Unsolved problems in far-infrared astronomy? • How do dusty, starburst galaxies assemble? • Where are luminous infrared galaxies today? • How do starbursts relate to dark matter? • What is the role of dust in star formation? • What is the connection between dusty star formation and AGNs? PACS PACS SPIRE SPIRE SPIRE Z=0 Z=1 Z=4 Herschel Extragalactic Surveys - Observe at SED peak - Bolometric far-IR luminosities - Large and uniform samples ANGULAR RESOLUTION SURVEY SPEED Herschel Science Motivation HERMES INFORMATION ON THE WEB: HERMES.SUSSEX.AC.UK AND HERSCHEL.UCI.EDU Asantha Cooray, UC Irvine Dusty Universe 2016 2000 ULIRGS Star-Formation 200 Rate in solar Herschel/SPIRE masses per year LIRGS 20 MILKY-WAY LIKE 2 (~Milky-way SFR) (i) ULIRGS typically have about ~1010 solar masses in stars (ii) So the time scale for star-formation is [M*/(dM*/dt)] ~ 100 Million years What kind of galaxies did we detect with Herschel? Asantha Cooray, UC Irvine Dusty Universe 2016 Optical Universe Infrared Universe major merger ULIRG AGN elliptical or heavy bombardment 1000 100/yr) o 10 SFR (M 1 0.1 0.5 Gyr 1 Gyr 1.5 Gyr 2.0 Gyr 2.5 Gyr e.g. Hopkins et al. 2009, Narayanan et al. 2009 What are Dusty Star Forming Galaxies? Illustration from Caitlin Casey Optical Universe Infrared Universe major merger ULIRG AGN elliptical or heavy bombardment Peak SFR “feedback 1000 processes?” Slow buildup exhausting of stellar 100/yr) SF fuel? o mass... Peak 10 SFR (M BH Phase old stellar population 1 0.1 0.5 Gyr 1 Gyr 1.5 Gyr 2.0 Gyr 2.5 Gyr Active ULIRG e.g. Hopkins et al. 2009, Phase Narayanan et al. 2009 T~100Myr What are Dusty Star Forming Galaxies? Illustration from Caitlin Casey Redshift distribution of SPIRE Sources? Alex Amblard et al. 2010 (ex-UCI postdoc; now NASA Ames) 102 101 z=0 z=1 z=4 100 −1 F (mJy) 10 10−2 10−3 100 101 102 103 (μm) Naive expectation based on the SED: The surface density of 350 μm selected S250 > S350 > S500: z < 2 sources (z~1.8 to 3) S350 > 20 mJy S250 <~ S350 > S500: z ~ 2 to 3 is ~800/deg2 S250 < S350 < S500: z > 4 Amblard et al. 2010 sub-mm colors as a mechanism to select z > 2 galaxies Redshift distribution of SPIRE Sources? 350μm selected galaxies > 5σ are at mostly at z = 2.2 ± 0.6 In red and blue additional color cuts on 500/250 ratio (red selects higher-z end with “redder” colors) The “statistical” redshift distribution implied by SPIRE colors for the 1686 The surface density of 350 m selected µ sources sources (z~1.8 to 3) S350 > 20 mJy [equivalent to fitting each SED with is ~800/deg2 a single-temp model and marginalizing over T,β] (Hughes et al 2002; Aretxaga et al. 2007) Amblard et al. 2010 Caitlin Casey et al. 2012 Redshift distribution of (ex-UCI postdoc; SPIRE Sources? UT Austin faculty) (LRIS sources) Keck LRIS/DEIMOS followup. z peak is around z~1 (250 micron dominated) ~1000 redshifts in the optical Redshift gap; z > 1.5 highly incomplete. Bethermin et al. 2012 N (>S) N N (>S) N ⨂ = Probability Flux mu Flux Intrinsic Source Count Magnification Cross Section Lensed Source Count Negrello et al. 2010 Science Julie Wardlow et al. 2013, ApJ (UCI ex-postdoc; Durham lecturer) Lensing galaxy selection at sub-mm wavelengths > 95% efficient The Nature of Brightest high-z Herschel Galaxies Asantha Cooray, UC Irvine Dusty Universe 2016 Bootes/NDWFS/SDWFS 16 sqr. degrees • Lensing: Flux boosted (magnified) • Can study fainter objects than usually available. • Can study spatial distribution of gas, dust, stars at higher resolution than with normal galaxies at the same distances. The Nature of Brightest high-z Herschel Galaxies Negrello et al. 2010 Science; Wardlow et al. 2012, ApJ; Bussman et al. 2012 ApJ Asantha Cooray, UC Irvine Dusty Universe 2016 Source CO Redshift GBT CARMA CSO High-Resolution Imaging Keck SMA JVLA Extensive Ground-based Follow-up Observations Asantha Cooray, UC Irvine Dusty Universe 2016 Jae Calanog UCI PhD 2014 We now have 100 images like these in total with Keck/LGS AO/HST Keck LGS-AO Imaging Fu et al. 2012; Bussmann et al. 2012; Fu et al. 2013; Calanog et al. 2014; Timmons et al. 2015 Asantha Cooray, UC Irvine Dusty Universe 2016 Planck H-ATLAS (brightest source) 550 μm 250-500 μm S250 = 320 ± 20 mJy S350 = 380 ± 60 mJy S550 = 1.07 ± 0.12 JY S500 = 300 ± 20 mJy S350 = 1.1 ± 0.2 JY ZCO = 3.26 CARMA A lensed Planck source resolved by Herschel (in ATLAS) Fu, Hai et al. 2012, ApJ Asantha Cooray, UC Irvine Dusty Universe 2016 LFIR = 1.6 X1013 L⊙ SFR ~ 1900 M⊙/yr TDUST = 62 ± 3 K 1 ARCSEC No evidence for AGN MDUST = 6 X108 M⊙ MSTARS = 3 X1010 M⊙ MGAS = 7 X1010 M⊙ MDYNAMICAL = 3 X1011 M⊙ Gas-rich (70% of baryons in gas) Young (MSTARS/SFR~20 Myr) Short Star-burst (MGAS/SFR~40 Myr) Hai Fu et al. 2012, ApJ (ex-UCI postdoc; Iowa faculty) A lensed Planck source resolved by Herschel (in ATLAS) Fu, Hai et al. 2012, ApJ Asantha Cooray, UC Irvine Dusty Universe 2016 H-ATLAS: 650 sq. degrees. ~2 lensed Planck CSC Starbursting knot in a sources. One in HerMES over 370 sq. degrees. spiral galaxy. Disk is mostly an old stellar population. Lensed optical arc Lensed Herschel-detected source (starbursting clump) 1” z=1.68, z determined from the Herschel-SPIRE/FTS spectrum with the 158 micron CII line George et al. 2014; Timmons et al. 2015 Nick Timmons UCI PhD 2017 Herschel Lensed Sources Asantha Cooray, UC Irvine Dusty Universe 2016 H-ATLAS: 650 sq. degrees. ~2 lensed Planck CSC Source reconstructed: SMA/JVLA (red) sources. One in HerMES over 370 sq. degrees. and Keck/Hubble (green/blue) n = 103 Galactic SF Regions L[C II ] /LCO(1 0) = 4100 Normal Galaxies n = 102 10− 2 StarburstNuclei n = 104 Local ULIRGs HATLAS J132427 LESS J033229.4 BR1202-0725 SMM J2135 5 FIR n = 10 HDF 850.1 /L ] HFLS 3 II − 3 [C 10 SDP.81 L ID 141 NBv1.43 n = 106 − 4 4 3 2 10 G0 = 10 G0 = 10 G0 = 10 10− 7 10− 6 10− 5 LCO(1 0) /LFIR 1” z=1.68, z determined from the Herschel-SPIRE/FTS spectrum with the 158 micron CII line George et al. 2014; Timmons et al. 2015 Herschel Lensed Sources Asantha Cooray, UC Irvine Dusty Universe 2016 Discovery in H-ATLAS during SDP: Negrello et al. 2010 Science z=0.3 elliptical (Sloan LRG) z=3.04 DSFG 2010 Keck+SMA 2015 HST+ALMA SDP.81 Asantha Cooray, UC Irvine Dusty Universe 2016 Dye et al. 2015 SDP.81 Negrello et al. 2010; Vlahakis et al. 2015; Dye et al. 2015; Swinbank et al. 2015;… (6 papers with ALMA) Asantha Cooray, UC Irvine Dusty Universe 2016 50 pc resolution in a z of 3 galaxy thanks to lensing + ALMA SDP.81 Negrello et al. 2010; Vlahakis et al. 2015; Dye et al. 2015; Swinbank et al. 2015;… (6 papers with ALMA) Asantha Cooray, UC Irvine Dusty Universe 2016 Promise of Herschel in Lensing Studies • ~0.2/sq. deg (S500>100 mJy) lensed source - identified ~90% efficiency. • Herschel extragalactic surveys: ~1200 sq. degrees, so ~250 lensed galaxies. • Compared to ~200 lensed galaxies now known in optical and radio 500 um peaked sources S250 < S350 < S500: z > 4? *Confusion reduced S(500) – fS(250) 250 um 350 um 500 um * HST WFC3+ACS 250 um 350 um 500 um * FLS3 z=6.34 Dowell et al. 2014 ApJ technique IRAM 1.1mm z = 6.34 Dusty Starburst Galaxy in HerMES Riechers, D. et al. Nature 2013; Cooray et al. 2014 Asantha Cooray, UC Irvine Dusty Universe 2016 250 um 350 um 500 um * ! Asantha Cooray, UC Irvine Dusty Universe 2016 z=2.1 z=6.3 Weakly lensed by two z=2.1 galaxies with magnification 12 LFIR = 6X10 L⊙ MDUST > 109 M⊙ 1.6 +/- 0.3 SFR ~ 1300 M⊙/yr MSTARS ~ 5X1010 M⊙ 11 TDUST = 55 ± 10 K MGAS ~ 10 M⊙ [G2 identification in R13 as K-band ID of FLS3 incorrect] No evidence for a quasar/massive AGN! z = 6.34 Dusty Starburst Galaxy in HerMES Riechers, D.
Recommended publications
  • 2020 July 09 Dr. Paul Hertz Astrophysics Director Science

    2020 July 09 Dr. Paul Hertz Astrophysics Director Science

    2020 July 09 Dr. Paul Hertz Astrophysics Director Science Missions Directorate National Aeronautics and Space administration (NASA) Dear Paul, The NASA Astrophysics Advisory Committee (APAC) had its Summer meeting on 2020 June 23-24. Due to the COVID-19 pandemic and related NASA operational and travel restriction (Stage 4), the entire two-days of the meeting where conducted virtually using WebExtm videoconferencing technology accompanied by dial-in phone lines. The following members of the APAC attended the meeting: Kelly Holley-Bockelman, Laura Brenneman, John Conklin (Vice Chair), Asantha Cooray, Massimiliano Galeazzi, Jessica Gaskin, Hashima Hasan (APAC Executive Secretary), William Jones, Suvrath Mahadevan, Margaret Meixner, Michael Meyer, Leonidas Moustakas, Lucianne Walkowitz, and Chick Woodward (APAC Chair). Public lines were opened, and Dr. Hasan began the meeting by welcoming all the APAC members, and explaining its purpose. Dr. Hasan reminded APAC members who had conflicts of interest with specific topics on the agenda that as conflicted members they were allowed to listen to the presentation but could not participate in the committee’s discussion. Dr. Hasan then reviewed the Federal Advisory Committee Act (FACA) rules. Dr. Woodward then welcomed the members to the meeting, outlined the agenda, and reiterated some of the FACA and conflict of interest rules. APAC members proceeded to introduce themselves. The agenda consisted of the following presentations: • Astrophysics Division Update – Paul Hertz • State of the Profession – Chick Woodward and the APAC Committee • ExoPAG, COPAG, and PhysPAG reports – Michael Meyer, Margaret Meixner, Graca Rocha • SOFIA update – Margaret Meixner, Naseem Rangwala • James Webb update – Eric Smith • ESCAPE update – Kevin France • Athena update – Rob Petre • GUSTO update – Chris Walker • COSI update – John Tomsick • CASE/ARIEL update – Mark Swain • Science Activation update – Kristen Erickson The APAC thanks all the presenters for their time and efforts to provide crisp and informative presentations.
  • Download This Article (Pdf)

    Download This Article (Pdf)

    244 Trimble, JAAVSO Volume 43, 2015 As International as They Would Let Us Be Virginia Trimble Department of Physics and Astronomy, University of California, Irvine, CA 92697-4575; [email protected] Received July 15, 2015; accepted August 28, 2015 Abstract Astronomy has always crossed borders, continents, and oceans. AAVSO itself has roughly half its membership residing outside the USA. In this excessively long paper, I look briefly at ancient and medieval beginnings and more extensively at the 18th and 19th centuries, plunge into the tragedies associated with World War I, and then try to say something relatively cheerful about subsequent events. Most of the people mentioned here you will have heard of before (Eratosthenes, Copernicus, Kepler, Olbers, Lockyer, Eddington…), others, just as important, perhaps not (von Zach, Gould, Argelander, Freundlich…). Division into heroes and villains is neither necessary nor possible, though some of the stories are tragic. In the end, all one can really say about astronomers’ efforts to keep open channels of communication that others wanted to choke off is, “the best we can do is the best we can do.” 1. Introduction astronomy (though some of the practitioners were actually Christian and Jewish) coincided with the largest extents of Astronomy has always been among the most international of regions governed by caliphates and other Moslem empire-like sciences. Some of the reasons are obvious. You cannot observe structures. In addition, Arabic astronomy also drew on earlier the whole sky continuously from any one place. Attempts to Greek, Persian, and Indian writings. measure geocentric parallax and to observe solar eclipses have In contrast, the Europe of the 16th century, across which required going to the ends (or anyhow the middles) of the earth.
  • Einstein, Eddington, and the Eclipse: Travel Impressions

    Einstein, Eddington, and the Eclipse: Travel Impressions

    EINSTEIN, EDDINGTON, AND THE ECLIPSE: TRAVEL IMPRESSIONS ESSAY 195 INTRODUCTION The total solar eclipse that occurred on 29 May 1919—perhaps considered the most famous solar eclipse ever—was exceptional for a variety of scientific, political, social, and even religious reasons. At just over five minutes of totality (more precisely, 302 seconds), it was a long eclipse. Behind the sun appeared the Taurus constellation, which included the Hyades, the brightest star cluster in the ecliptic. The preparations of the British teams that observed it, and which are the subject of this essay, took place in the middle of the Great War, during a period of international instability. The observation locations selected by these specialists were in the tropics, in distant regions unknown to most astronomers, and thus required extensive preparations. These places included the city of Sobral, in the north-eastern state of Ceará in Brazil, and the equatorial island of Príncipe, then part of the Portuguese empire, and today part of the Republic of São Tomé and Príncipe. Located in the Gulf of Guinea on the West African coast, Príncipe was then known as one of the world’s largest cocoa producers, and was under international suspicion for practicing slave labour. Additionally, among the teams of expeditionary astronomers from various countries—including the United Kingdom, the United States, and Brazil—there was not just one, but two British teams. This was an uncommon choice given the material, as well as the scientific and financial effort involved, accentuated by the unfavourable context of the war. The expedition that observed at Príncipe included Arthur Stanley Eddington (1882– 1944), the astrophysicist and young director of the Cambridge Observatory, as well as the clockmaker and calculator Edwin Turner Cottingham (1869–1940); the expedition that visited Brazil included Andrew Claude de la Cherois Crommelin (1865–1939), and Charles Rundle Davidson (1875–1970), both experienced astronomers at the Greenwich Observatory (see pp.
  • Gravitational Time Delay Effects on Cosmic Microwave Background Anisotropies

    Gravitational Time Delay Effects on Cosmic Microwave Background Anisotropies

    PHYSICAL REVIEW D, VOLUME 63, 023504 Gravitational time delay effects on cosmic microwave background anisotropies Wayne Hu* Institute for Advanced Study, Princeton, New Jersey 08540 and Department of Astronomy and Astrophysics, University of Chicago, Chicago, Illinois 60637 Asantha Cooray† Department of Astronomy and Astrophysics, University of Chicago, Chicago, Illinois 60637 ͑Received 2 August 2000; published 18 December 2000͒ We study the effect of gravitational time delay on the power spectra and bispectra of the cosmic microwave background ͑CMB͒ temperature and polarization anisotropies. The time delay effect modulates the spatial surface at recombination on which temperature anisotropies are observed, typically by ϳ1 Mpc. While this is a relatively large shift, its observable effects in the temperature and polarization fields are suppressed by geometric considerations. The leading order effect is from its correlation with the closely related gravitational lensing effect. The change to the temperature-polarization cross power spectrum is of order 0.1% and is hence comparable to the cosmic variance for the power in the multipoles around lϳ1000. While unlikely to be extracted from the data in its own right, its omission in modeling would produce a systematic error comparable to this limiting statistical error and, in principle, is relevant for future high precision experiments. Contributions to the bispectra result mainly from correlations with the Sachs-Wolfe effect and may safely be neglected in a low density universe. DOI: 10.1103/PhysRevD.63.023504 PACS number͑s͒: 98.80.Es, 95.85.Nv I. INTRODUCTION small effects can accumulate along the path. Indeed it is well known that the gravitational lensing of CMB photons has a In order that the full potential of anisotropies in the cos- substantial effect on the power spectrum of the anisotropies mic microwave background ͑CMB͒ temperature and polar- ͓11,12͔.
  • Proceedings of Spie

    Proceedings of Spie

    PROCEEDINGS OF SPIE SPIEDigitalLibrary.org/conference-proceedings-of-spie Overview of the Origins Space telescope: science drivers to observatory requirements Margaret Meixner, Lee Armus, Cara Battersby, James Bauer, Edwin Bergin, et al. Margaret Meixner, Lee Armus, Cara Battersby, James Bauer, Edwin Bergin, Asantha Cooray, Jonathan J. Fortney, Tiffany Kataria, David T. Leisawitz, Stefanie N. Milam, Klaus Pontoppidan, Alexandra Pope, Karin Sandstrom, Johannes G. Staguhn, Kevin B. Stevenson, Kate Y. Su, Charles Matt Bradford, Dominic Benford, Denis Burgarella, Sean Carey, Ruth C. Carter, Elvire De Beck, Michael J. Dipirro, Kimberly Ennico-Smith, Maryvonne Gerin, Frank P. Helmich, Lisa Kaltenegger, Eric. E. Mamajek, Gary Melnick, Samuel Harvey Moseley, Desika Narayanan, Susan G. Neff, Deborah Padgett, Thomas L. Roellig, Itsuki Sakon, Douglas Scott, Kartik Sheth, Joaquin Vieira, Martina Wiedner, Edward Wright, Jonas Zmuidzinas, "Overview of the Origins Space telescope: science drivers to observatory requirements," Proc. SPIE 10698, Space Telescopes and Instrumentation 2018: Optical, Infrared, and Millimeter Wave, 106980N (24 July 2018); doi: 10.1117/12.2312255 Event: SPIE Astronomical Telescopes + Instrumentation, 2018, Austin, Texas, United States Downloaded From: https://www.spiedigitallibrary.org/conference-proceedings-of-spie on 23 Aug 2019 Terms of Use: https://www.spiedigitallibrary.org/terms-of-use Overview of the Origins Space Telescope: Science Drivers to Observatory Requirements Margaret Meixnera,b,c, Lee Armusd, Cara Battersbye, James Bauerf, Edwin Berging, Asantha Coorayh, Jonathan J. Fortneyi, Tiffany Katariaj, David T. Leisawitzc, Stefanie N. Milamc, Klaus Pontoppidana, Alexandra Popek, Karin Sandstroml, Johannes G. Staguhnb,c, Kevin B. Stevensona, Kate Y. Sum, Charles Matt Bradfordj, Dominic Benfordn, Denis Burgarellao, Sean Careyd, Ruth C.
  • Hubble Sees Light Bending Around Nearby Star : Nature News

    Hubble Sees Light Bending Around Nearby Star : Nature News

    NATURE | NEWS Hubble sees light bending around nearby star Rare astronomical observation shows effects of relativity. Alexandra Witze 07 June 2017 STSI Stein 2051 B is a white-dwarf star in the constellation Camelopardalis. The Hubble Space Telescope has spotted light bending because of the gravity of a nearby white dwarf star — the first time astronomers have seen this type of distortion around a star other than the Sun. The finding once again confirms Einstein’s general theory of relativity. A team led by Kailash Sahu, an astronomer at the Space Telescope Science Institute in Baltimore, Maryland, watched the position of a distant star jiggle slightly, as its light bent around a white dwarf in the line of sight of observers on Earth. The amount of distortion allowed the researchers to directly calculate the white dwarf’s mass — 67% that of the Sun. “It’s a very difficult observation with a really nice result,” says Pier-Emmanuel Tremblay, an astrophysicist at the University of Warwick in Coventry, UK, who was not involved in the discovery. The findings were published in Science 1 and presented at a meeting of the American Astronomical Society in Austin, Texas, on 7 June. White dwarfs are the remains of stars that have finished burning their nuclear fuel. The Sun will eventually become one. Sahu’s team studied a white dwarf known as Stein 2051 B, in the constellation Camelopardalis. At 5 parsecs (17 light years) from Earth, it is the sixth-nearest white dwarf. Because it is so close, it appears to move quickly across the sky compared with more-distant stars.
  • Smart Optics for ESA Space Science Missions

    Smart Optics for ESA Space Science Missions

    Smart Optics for ESA Space Science Missions • Gaia, JWST, Darwin • Scientific objectives • Payload description • Optical technology developments Dr. Ph. Gondoin (ESA) ESA’s IR and visible astronomy missions DARWIN GAIA Herschel Planck Eddington JWST 1 GAIA Science Objectives Understanding the structure and evolution of the Galaxy, i.e.: – census of the content of a large part of the Galaxy – quantification of the present spatial structure from distance (3-D map) – knowledge of the 3-D space motions Æ Complementary astrometry, photometry and radial velocities: – Astrometry: distance and tranverse kinematics – Photometry: extinction, intrinsic luminosity, abundances, ages, – Radial velocities: 3-D kinematics, gravitational forces, mass distribution, stellar orbits GAIA (compared with Hipparcos) Hipparcos GAIA Magnitude limit 12 20-21 mag Completeness 7.3 – 9.0 ~20 mag Bright limit ~0 ~3-7 mag Number of objects 120 000 26 million to V = 15 250 million to V = 18 1000 million to V = 20 Effective distance limit 1 kpc 1 Mpc Quasars None ~5 ×105 Galaxies None 106 - 107 Accuracy ~1 milliarcsec 4 µarcsec at V = 10 10 µarcsec at V = 15 200 µarcsec at V = 20 Broad band 2-colour (B and V) 4-colour to V = 20 Mediumphotometry band None 11-colour to V = 20 Radialphotometry velocity None 1-10 km/s to V = 16-17 Observing programme Pre-selected On-board and unbiased 2 PayloadGAIA payload • 2 astrometric telescopes: • Separated by 106o • SiC mirrors (1.4 m × 0.5 m) • Large focal plane (TDI operating CCDs) • 1 additional telescope equipped with: • Medium-band photometer • Radial-velocity spectrometer Optical technology for GAIA • CCD’s and focal plane technology: (ASTRIUM.GB+E2V under ESA TRP contract) – Astrometry: 3 side buttable, small pixel (9 µm), high perf.
  • Travelling Back Through Time COORAYDR ASANTHA

    Travelling Back Through Time COORAYDR ASANTHA

    Travelling back through time DR ASANTHA COORAY With Drs Julie Wardlow and Joseph Smidt from his research group, Professor Asantha Cooray describes the areas of study by which they are seeking to expand knowledge of far distant galaxies and star formation Can you begin by outlining your research goals? Cooray: The fi rst goal for my team is to search for the fi rst galaxies in the distant, early Universe. The fi rst galaxies are expected to be small in size and mass compared to later ones and their distance at almost the edge of the observable Universe makes them hard to see individually with existing observatories. So we look for signals in the sky that suggest their presence through aggregate effects, such as small variations in the total light emitted by them. Such searches for fi rst galaxies are best done at short infrared (like a galaxy), a foreground mass (such as wavelengths in the electromagnetic spectrum. another galaxy, or a cluster of galaxies) and A second research goal is to study the dust- our telescopes on Earth. The light from the enshrouded star formation in distant galaxies. background source has to pass through, or Since optical light is absorbed by dust, such very close to, the foreground mass in order observations are best done at long infrared to reach us. However, as Einstein theorised, wavelengths again from space. Why is there a need to investigate zodiacal the path that light takes is affected by the dust cloud? How does the Zodiacal dust, intervening mass, in much the same way as How will infrared wavelengths further Extragalactic Background and Reionisation light is defl ected by the lens in spectacles.
  • The Atmospheric Remote-Sensing Infrared Exoplanet Large-Survey

    The Atmospheric Remote-Sensing Infrared Exoplanet Large-Survey

    ariel The Atmospheric Remote-Sensing Infrared Exoplanet Large-survey Towards an H-R Diagram for Planets A Candidate for the ESA M4 Mission TABLE OF CONTENTS 1 Executive Summary ....................................................................................................... 1 2 Science Case ................................................................................................................ 3 2.1 The ARIEL Mission as Part of Cosmic Vision .................................................................... 3 2.1.1 Background: highlights & limits of current knowledge of planets ....................................... 3 2.1.2 The way forward: the chemical composition of a large sample of planets .............................. 4 2.1.3 Current observations of exo-atmospheres: strengths & pitfalls .......................................... 4 2.1.4 The way forward: ARIEL ....................................................................................... 5 2.2 Key Science Questions Addressed by Ariel ....................................................................... 6 2.3 Key Q&A about Ariel ................................................................................................. 6 2.4 Assumptions Needed to Achieve the Science Objectives ..................................................... 10 2.4.1 How do we observe exo-atmospheres? ..................................................................... 10 2.4.2 Targets available for ARIEL ..................................................................................
  • Stellar Structure and Habitable Planet Finding

    Stellar Structure and Habitable Planet Finding

    SP-538 January 2004 Second Eddington Workshop Stellar Structure and Habitable Planet Finding 9-11 April 2003 Palermo, Italy SUB Gottingen 7 212 196 901 Organised by European Space Agency and INAF — Osservatorio Astronomico di Palermo European Spate Agenty Agente spatiale europeenne CONTENTS Preface ix Oral Papers The Eddington baseline mission, F. Favata 3 Models of stellar structure for asteroseismology, F. D'Antona, J. Montalban, I. Mazz- itelli 13 Eddington and the internal constitution of the stars, I. W. Roxburgh 23 Science requirements and their translation into instrumental design, C. Catala, A. Aricha, 0. Boulade, E. Diaz, G. Epstein, F. Favata, K. Home, H. Kjeldsen, D. Lumb, M. Mas-Hesse, 1. Roxburgh 39 CCD selection for Eddington, D. Lumb 47 Laboratory tests of Eddington photometry, D. M. Walton, G. Ramsay, A. Smith 51 The Eddington CCD data simulator, T. Arentoft, H. Kjeldsen, J. De Ridder, D. Stello 59 The Eddington light curve simulator, J. De Ridder, H. Kjeldsen, T. Arentoft, A. Claret 67 Choosing the proper transit detection algorithm for Eddington, B. Tingley 71 The nature of OGLE transiting planet candidates, J. Eisloffel, M. Kiirster, A. P. Hatzes, E. Guenther 81 Asteroseismology and extrasolar planets of K Giants, A. P. Hatzes, J. Setiawan, L. Pasquini, L. da Silva 87 The Sun as a reference for Eddington, S. Turck-Chieze 95 Pulsating pre-main sequence stars as possible Eddington targets, K. Zwintz, W. W. Weiss 105 Mode extraction from time series: from the challenges of COROT to those of Edding- ton,T. Appourchaux, O. Moreira, G. Berthomieu, T. Toutain 109 Colour information in asteroseismology, R.
  • 1.7 News & Views MH

    1.7 News & Views MH

    news and views lifetimes. In the longer run, the experience 1. Claverie, A., Isaak, G. R., McLeod, C. P., van der Raay, H. B. & that cancers with different EGFR mutations gained with MOST on the nature of stellar Roca Cortes, T. Nature 282, 591–594 (1979). may respond differently to inhibitors7. 2. Grec, G., Fossat, E. & Pomerantz, M. Nature 288, 541–544 pulsations, as well as on optimal techniques (1980). Finally, in cancers that initially respond and for space-based photometry,will be of crucial 3. Matthews, J. M. et al. Nature 430, 51–53 (2004). subsequently recur,the EGFR gene will be the importance to coming asteroseismic missions 4. Goldreich, P. & Keeley, D. A. Astrophys. J. 212, 243–251 (1977). first place to look for additional mutations — such as the French-based COROT mission 5. Christensen-Dalsgaard, J. & Frandsen, S. Solar Phys. 82, that have conferred drug resistance. 469–486 (1983). and, one may hope, the far more ambitious 6. Kjeldsen, H. & Bedding, T. R. Astron. Astrophys. 293, 87–106 How will these observations be translated Eddington mission originally selected for (1995). into clinical practice? EGFR mutations are (but currently not included in) the pro- 7. Brown, T. M., Gilliland, R. L., Noyes, R. W. & Ramsey, L. W. more common in women who have never ■ Astrophys. J. 368, 599–609 (1991). gramme of the European Space Agency. 8. Martic, M., Lebrun, J.-C., Appourchaux, T. & Korzennik, S. G. smoked. Overall, however, fewer than 10% of Jørgen Christensen-Dalsgaard and Hans Kjeldsen Astron. Astrophys. 418, 295–303 (2004). lung adenocarcinomas in patients in the are in the Department of Physics and Astronomy, 9.
  • Heterodyne Receiver for Origins

    Heterodyne Receiver for Origins

    Heterodyne Receiver for Origins a, b c Martina C. Wiedner , * Susanne Aalto, Edward G. Amatucci , d e f g Andrey Baryshev, Cara Battersby , Victor Belitsky, Edwin A. Bergin, h c i j Bruno Borgo, Ruth C. Carter, Emmanuel Caux , Asantha Cooray, c b a f James A. Corsetti, Elvire De Beck , Yan Delorme, Vincent Desmaris, c k l Michael J. DiPirro, Brian Ellison , Anna M. Di Giorgio, m n a Martin Eggens , Juan-Daniel Gallego , Maryvonne Gerin , o p m,q Paul F. Goldsmith , Christophe Goldstein, Frank Helmich , r s t,u Fabrice Herpin , Richard E. Hills , Michiel R. Hogerheijde , v m m a Leslie K. Hunt , Willem Jellema , Geert Keizer, Jean-Michel Krieg, w x p c Gabby Kroes, Philippe Laporte, André Laurens, David T. Leisawitz , a,o c o Dariusz C. Lis , Gregory E. Martins, Imran Mehdi, c,y,z aa c Margaret Meixner, Gary Melnick, Stefanie N. Milam , z h ab David A. Neufeld, Napoléon Nguyen Tuong, René Plume, y r Klaus M. Pontoppidan , Benjamin Quertier-Dagorn, ac,ad c,z aa Christophe Risacher , Johannes G. Staguhn , Edward Tong, ae ac Serena Viti, Friedrich Wyrowski, and † The Origins Space Telescope Mission Concept Study Team aLaboratoire d’Etudes du Rayonnement et de la Matière en Astrophysique et Atmosphères (LERMA), Observatoire de Paris, Université Paris Sciences & Lettres (PSL) Centre National de la Recherche Scientifique (CNRS), Sorbonne Université, Paris, France bChalmers University of Technology, Department of Space, Earth and Environment, Onsala Space Observatory, Onsala, Sweden cNASA Goddard Space Flight Center, Greenbelt, Maryland, United