Observations of DCO + : Tracing the abundance of CO and N 2 in prestellar. cores. Laurent Pagani LERMA, UMR8112 du CNRS, Observatoire de Paris
|
|
- Griffin Neal Robbins
- 8 years ago
- Views:
Transcription
1 Observations of DCO + : Laurent Pagani LERMA, UMR8112 du CNRS, Observatoire de Paris Tracing the abundance of CO and N 2 in prestellar L183 - Spitzer/IRAC4-8 µm cores with the contribution of A. Bourgoin & F. Lique
2 OVERVIEW (1)Deuteration & ortho-h 2 deuteration control (2)CO & N 2 : how to trace them? (3)Conclusions
3 OVERVIEW (1)Deuteration & ortho-h 2 deuteration control (2)CO & N 2 : how to trace them? (3)Conclusions 3
4 (1)Deuteration & ortho-h 2 deuteration control Deuteration in a nutshell (ζ,uv) + H H + + e - H + + D D + + H D + + H 2 HD + H +ΔE HD becomes the deuterium reservoir: HD/H 2 3 x 10-5 (ζ,uv) + H2 H2 + + e - H2 + + H2 H3 + + H H3 + is the starting point of the cold phase ion-neutral chemistry H HD H 2 D + + H K H CO HCO + + H 2 Deuteration is favored in the coldest environment H 2 D + + CO DCO + + H 2 HCO + + HD, X[H 2 D + ] = X[H 3 +] (Pagani et al. 1992) (while D/H , Linsky et al. 2007) H 2 D + + N2 N2D + + H 2 N2H + + HD, H 2 D + D 2 H + D 3 + 4
5 (1)Deuteration & ortho-h 2 deuteration control Detection of D 2 CO, ND 2 H, D 2 O, CD 2 OH, Detection of ND 3 and CD 3 OH : need for D 2 H + and D 3 + (Lis et al. 2002, Roberts et al. 2003) H HD H 2 D + + HD D 2 H + + HD H 2 D + + H K D 2 H + + H K D H K At low T kin, reactions only to the right! (Giles et al. 1992) But... 2 spin states per species (ortho & para), 3 spin states for D3 + o-h2 = p-h K o-h 2 D + = p-h 2 D K p-d 2 H + = o-d 2 H K etc.
6 (1)Deuteration & ortho-h 2 deuteration control H HD H 2 D + + H K??? p-h HD p-h 2 D + + p-h K p-h HD o-h 2 D + + p-h K p-h HD p-h 2 D + + o-h K p-h HD o-h 2 D + + o-h 2-25 K etc. p-h 2 D + + o-h 2 o-h 2 D + + p-h K o-h 2 controls the deuteration process! Pagani et al. 1992, 2009, Flower et al. 2006
7 (1)Deuteration & ortho-h 2 deuteration control ζ = s -1 ζ = s -1 ζ = s -1 X[e - ] X[CO] = 10-5 n(h 2 ) = cm -3 N 2 D + /N 2 H + ratio X[CO] = 10-6 n(h 2 ) = cm -3 o/p H 2 limited depletion ortho - H 2 > 1 % no H 2 D + Pagani et al. 2009
8 (1)Deuteration & ortho-h 2 deuteration control Ortho-H 2 : fabrication/destruction H 2 only fabricated on grains with o/p ratio = 3:1 ortho-h 2 destroyed via (Dalgarno et al. 1973, Le Bourlot 1991, Flower et al. 2006) : o-h 2 + H + p-h 2 + H + (Honvault et al. PRL 11+PCCP 11) o-h 2 + H + 3 p-h 2 + H + 3 (Hugo et al. 09, Crabtree et al. 11)
9 (1)Deuteration & ortho-h 2 deuteration control 1.5 My! Full chemical model OSU/Nahoon style + H 2 and H 3 + spin state chemistry Density = 10 4 cm -3 Pagani, Roueff & Lesaffre, 2012
10 (2)CO & N 2 : how to trace them? (1)Deuteration & ortho-h 2 deuteration control (2)CO & N 2 : how to trace them? (3)Conclusions
11 (2)CO & N 2 : how to trace them? 1) Atoms and grains condensate 2) H2 forms on grains 3a) UV is stopped 3b) Temperature drops 4) Molecules form 5) Water freezes on grains 6) Cores form & depletion appears Prediction : Herbst & Klemperer st Observation : Lemme et al B68 C 18 O N 2 H AND C 18 ODEPLETIONINCOLDDARKCLOUD N2H + Vol.570 C 18 O Bergin et al (a) ComparisonofC 18 O J p 1 0 integrated emission (contours) in B68 superposed on a map of visual extinction derived by ALL01 and convolved AM resolution. The C Ocontoursbeginat0.2Kkms andstepinunitsof0.1kkms.thea V imageisscaledfrom0to27mag.(b) Comparison 1 1 J p 1 0 integrated emission (contours) and the visual extinction image. The N 2 H contours begin at 0.3 K km s and step in units of 0.2 K km s. aps were referenced to a p 17 h 22 m 38 ṣ 2 and d p (J2000). The peak is located 6 east and 12 south of this position. A V AV Pagani et al with the visual extinction data using the techniques first edjeudi in Lada 11 etjuillet al. (1994). 13 For C 18 O, there is little scatter, thin C 17 O emission ( t 0.4), shown as an inset in the lower right-hand corner of Figure 1b, displays similar behavior and
12 (2)CO & N2: how to trace them? + N2H traces the dense gas Coreshine Pagani et al Steinacker et al (3.6 µm Spitzer/IRAC) 12
13 12 Problem : core CO emission masked by envelope emission & N2 is not measurable! L. Pagani et al.: L1506 : a prestellar core in the making 3 ig. 2. Left: lowresolution 13 CO (J:1 0) integrated intensity map of the L1506 Taurus cloud filament(originaldatafromnercessianetal.1988). ontour levels are 0.5 to 4.5 K km s 1 by steps of 1 K km s 1.ThePOM-12.5-mdishhasa4.5 resolution as shown in the bottom right corner. he square indicates the surface mapped in C 18 O(J:2 1).Theoffsets are with respect to L1506C coordinates (see text). Right:thesmoothedC 18 O :2 1) integrated intensity map. Superposed to the map is the strip path observed with PRONAOS (Stepnik et al. 2003) along which we observed CO, C 18 O, and N 2 H + with a good signal to noise ratio (see Fig. 3). The crosses indicate the observed points and the 3 white boxes (superposed 3 crosses) the points observed also in C 17 O(seeFig.5).Thedegraded30-mbeamsizeisrepresented.Levels are from 0.1 to 0.7 K km s 1 by eps of 0.1 K km s 1.The(0,0)positioncorrespondstoα 2000 = 4 h 18 m 50 s δ 2000 = see Figure 13. Blue diamonds represent the location of the lowest χr 2, note they are in averaged since it is focused only on the central region of each core. (2)CO & N 2 : how to trace them? one of these cores is significantly depleted holds even taking into account reasonable variances in outer radius, temperature, and canonical abundance. In no case did we find varying any of these parameters substantially affected the results. This work is unique in that we have tested a more complete parameter space of r d, f d,andc 18 Ocanonicalabundancethanpreviously published work. While outer radius does not impact our results, choices of temperature Brady-Ford profile& and Shirley, canonical 2011 abundance : can. Even fixing these parameters, we cannot, however, robustly distinguish between a factor of 10 depletion and a factor of 1000 in f d,astheχr 2 are very similar (e.g., Figures 15, 10, and 11). In contrast, the depletion radius, r d,forsomeofourcoresis more strongly constrained than f d ;however,r d values for many of these cores are separated by little more than a beam width, and four of the cores have the same value for r d.workbylee et al. (2003) alsofoundf d hard to constrain. At the distance of Taurus, information in the HHT maps contains information on scales larger than θ mb /2 = 2100 AU. Greater spatial resolution would better constrain r d.improved resolution may even help constrain f d.forinstance,futureobservations with the 50 m Large Millimeter Telescope operating at 1.3 mm would increase our resolution by a factor of five. The difficulty in determining the absolute value of f d limits our Fig. 3. Spectra taken along the PRONAOS cut (see Fig. 2). The upper row shows the 13 CO (J:1 0) spectra. The middle L1506C row shows the C 18 O(J:1 0)spectra.Thelowerrow shows the N 2 H + (J:1 0) spectra. The velocity scale is 6.5 to 8 km s 1 for 13 CO and C 18 O, and 5.5 to 9 km s 1 Pagani et al for N 2 H +. Offsets increase from 13
14 (2)CO & N 2 : how to trace them? DCO + peaks in the cores! 1995ApJ B - CO disappears - DCO + appears - DCO + daughter of CO trouble? No! Solution! (Butner et al. 1995) 14
15 (2)CO & N 2 : how to trace them? Ø [CO] = & [HD] = Ø H HD H 2 D + + H 2 ( 20 %) Ø H CO HCO + + H 2 ( 80 %) Ø H 2 D + + CO HCO +, DCO + + HD, H 2 [H 2 D + ][CO] cst [DCO + ] cst So, we can have DCO + in a CO-depleted core
16 (2)CO & N 2 : how to trace them? Steady-state model Pagani, Roueff & Lesaffre, 2012
17 (2)CO & N 2 : how to trace them? A full chemical model to relate CO & DCO + and N2 & N2D +? Initial conditions? Sensitivity to parameters? Measurable Balance H CO HCO + + H 2 (100%) H 2 D + + CO DCO + + H 2 (33%) HCO + + HD (66%) D 2 H + + CO HCO + + D 2 (33%) DCO + + HD (66%) D CO DCO + + D 2 (100%) H N2 N2H + + H 2 (100%) H 2 D + + N2 N2D + + H 2 (33%) N2H + + HD (66%) D 2 H + + N2 N2H + + D 2 (33%) N2D + + HD (66%) D N2 N2D + + D 2 (100%) DCO + HCO + N2D + N2H + N2D +, N2H + + CO N2 + DCO +, HCO + 17
18 (2)CO & N 2 : how to trace them? N 2 H +, N 2 D +, and H 2 D + cut and fit CORE N 2 H + CORE N 2 D + H 2 D +
19 (2)CO & N 2 : how to trace them? Low gas temperature and N2D + /N2H + profile, ratio and depletion Pagani et al
20 (2)CO & N 2 : how to trace them? DCO + L183 Observations N2D + 20
21 (2)CO & N 2 : how to trace them? DCO + L183 Observations N2D + Relative abundances 21
22 (2)CO & N 2 : how to trace them? L183 : CO and N 2 abundances GBT CO depletion : 400 inside the core, 2000 from undepleted envelope? N2 depletion : 20 inside the core A possible explanation : CN not depleted in L183 (Hily-Blant, 2008, 2010) CN + N N2 + C could compensate for N2 depletion! Pagani et al
23 (2)CO & N 2 : how to trace them? L183 : CO and N 2 abundances GBT CO depletion : 400 inside the core, 2000 from undepleted envelope? N2 depletion : 20 inside the core A possible explanation : CN not depleted in L183 (Hily-Blant, 2008, 2010) CN + N N2 + C could compensate for N2 depletion! Pagani et al
24 (1)Deuteration & ortho-h 2 deuteration control (2)CO & N 2 : how to trace them? (3)Conclusions
25 D Chemistry is very sensitive to conditions: it can help to trace them and trace the history of star formation (Pagani, Roueff & Lesaffre, 2012; Pagani et al. 2013) D Chemistry must treat all spin states separately + state-to-state chem. (Pagani et al. 1992, Flower et al., 2006, Pagani et al. 2009, Hugo et al. 2009) Ortho-H 2 is the key species in H 3 +-carried Deuterium chemistry Ortho-H 2 is abundant outside prestellar cores (> 10%) and drops inside (< 1%) (Pagani et al. 2009) Steady-state is normally not possible : too much deuteration (DCO + everywhere, N2D + /N2H + >> 1,...) Deuterium chemistry helps to trace CO and N2 detailled depletion profiles CO depletion over 2000? (3)Conclusions N2 depletion compensated by in-situ formation? (Pagani, Bourgoin, Lique, 2012, A&A, 548, L4) Thank you for your attention
The Chemical Composition of a Molecular Cloud at the Outer Edge of the Galaxy
Carnegie Observatories Astrophysics Series, Vol. 4: Origin and Evolution of the Elements, 2003 ed. A. McWilliam and M. Rauch (Pasadena: Carnegie Observatories, http://www.ociw.edu/ociw/symposia/series/symposium4/proceedings.html)
More informationIV. Molecular Clouds. 1. Molecular Cloud Spectra
IV. Molecular Clouds Dark structures in the ISM emit molecular lines. Dense gas cools, Metals combine to form molecules, Molecular clouds form. 1. Molecular Cloud Spectra 1 Molecular Lines emerge in absorption:
More informationSearching for young proto-planetary disks from ALMA archival data Final presentation
Searching for young proto-planetary disks from ALMA archival data Final presentation Speaker: Pou Ieng Cheong( 張 寶 瑩 ) 1 Supervisor: Shih Ping Lai( 賴 詩 萍 ) 2,3 1 Department of electrophysics, NCTU 2 Department
More informationResultados Concurso Apex 2014-A
Resultados Concurso Apex 2014-A Propuesta: 2014A/04 Investigador Principal: Guido Garay, Universidad de Chila Título: SuperMALT: determining the physical and chemical evolution of high-mass starforming
More information8.1 Radio Emission from Solar System objects
8.1 Radio Emission from Solar System objects 8.1.1 Moon and Terrestrial planets At visible wavelengths all the emission seen from these objects is due to light reflected from the sun. However at radio
More informationCOMPARISON OF GAS AND DUST COOLING RATES IN NEARBY GALAXIES
IC 10 Henize 2-10 NGC 253 COMPARISON OF GAS AND DUST COOLING RATES IN NEARBY GALAXIES E.Bayet: LRA-LERMA-ENS (Paris) Antennae IC 342 M 83 NGC 6946 INTRODUCTION : OBJECTS : warm and dense molecular clouds
More informationHeating & Cooling in Molecular Clouds
Lecture 8: Cloud Stability Heating & Cooling in Molecular Clouds Balance of heating and cooling processes helps to set the temperature in the gas. This then sets the minimum internal pressure in a core
More informationSolar System science with the IRAM interferometer. Recent Solar System science with the IRAM Plateau de Bure interferometer
Recent Solar System science with the IRAM Plateau de Bure interferometer J. Boissier (Institut de radioastronomie millimétrique) Contact: boissier@iram.fr Outline Planet moons Io Titan Planets Mars Comets
More informationGIANT FREQUENCY SHIFT OF INTRAMOLECULAR VIBRATION BAND IN THE RAMAN SPECTRA OF WATER ON THE SILVER SURFACE. M.E. Kompan
GIANT FREQUENCY SHIFT OF INTRAMOLECULAR VIBRATION BAND IN THE RAMAN SPECTRA OF WATER ON THE SILVER SURFACE M.E. Kompan Ioffe Institute, Saint-Peterburg, Russia kompan@mail.ioffe.ru The giant frequency
More informationThe Four Questions to Ask While Interpreting Spectra. 1. How many different environments are there?
1 H NMR Spectroscopy (#1c) The technique of 1 H NMR spectroscopy is central to organic chemistry and other fields involving analysis of organic chemicals, such as forensics and environmental science. It
More informationLecture 3 Properties and Evolution of Molecular Clouds. Spitzer space telescope image of Snake molecular cloud (IRDC G11.11-0.11
Lecture 3 Properties and Evolution of Molecular Clouds Spitzer space telescope image of Snake molecular cloud (IRDC G11.11-0.11 From slide from Annie Hughes Review CO t in clouds HI: Atomic Hydrogen http://www.atnf.csiro.au/research/lvmeeting/magsys_pres/
More informationFrom lowest energy to highest energy, which of the following correctly orders the different categories of electromagnetic radiation?
From lowest energy to highest energy, which of the following correctly orders the different categories of electromagnetic radiation? From lowest energy to highest energy, which of the following correctly
More informationNGUYEN LUONG QUANG. Président du jury: J. Le Bourlot Rapporteurs: H. Beuther, T. Moore Examinateurs: I. Bonnell, F. Boulanger, F. Combes, F.
NGUYEN LUONG QUANG Supervisors: Frédérique Motte (CEA Saclay) Marc Sauvage (CEA Saclay) Président du jury: J. Le Bourlot Rapporteurs: H. Beuther, T. Moore Examinateurs: I. Bonnell, F. Boulanger, F. Combes,
More informationProton Nuclear Magnetic Resonance Spectroscopy
Proton Nuclear Magnetic Resonance Spectroscopy Introduction: The NMR Spectrum serves as a great resource in determining the structure of an organic compound by revealing the hydrogen and carbon skeleton.
More informationApplication of a New Immobilization H/D Exchange Protocol: A Calmodulin Study
Application of a New Immobilization H/D Exchange Protocol: A Calmodulin Study Jiang Zhao; Mei Zhu; Daryl E. Gilblin; Michael L. Gross Washington University Center for Biomrdical and Bioorganic Mass Spectrometry:
More informationSound. References: L.D. Landau & E.M. Lifshitz: Fluid Mechanics, Chapter VIII F. Shu: The Physics of Astrophysics, Vol. 2, Gas Dynamics, Chapter 8
References: Sound L.D. Landau & E.M. Lifshitz: Fluid Mechanics, Chapter VIII F. Shu: The Physics of Astrophysics, Vol., Gas Dynamics, Chapter 8 1 Speed of sound The phenomenon of sound waves is one that
More informationFundamentals of modern UV-visible spectroscopy. Presentation Materials
Fundamentals of modern UV-visible spectroscopy Presentation Materials The Electromagnetic Spectrum E = hν ν = c / λ 1 Electronic Transitions in Formaldehyde 2 Electronic Transitions and Spectra of Atoms
More informationSolar Energy. Outline. Solar radiation. What is light?-- Electromagnetic Radiation. Light - Electromagnetic wave spectrum. Electromagnetic Radiation
Outline MAE 493R/593V- Renewable Energy Devices Solar Energy Electromagnetic wave Solar spectrum Solar global radiation Solar thermal energy Solar thermal collectors Solar thermal power plants Photovoltaics
More informationRemote Sensing of Clouds from Polarization
Remote Sensing of Clouds from Polarization What polarization can tell us about clouds... and what not? J. Riedi Laboratoire d'optique Atmosphérique University of Science and Technology Lille / CNRS FRANCE
More information6) How wide must a narrow slit be if the first diffraction minimum occurs at ±12 with laser light of 633 nm?
Test IV Name 1) In a single slit diffraction experiment, the width of the slit is 3.1 10-5 m and the distance from the slit to the screen is 2.2 m. If the beam of light of wavelength 600 nm passes through
More informationHighlights from the VLA/ANGST Survey
Highlights from the VLA/ANGST Survey Evan Skillman U. Minnesota Gas in Galaxies 2011: From Cosmic Web to Molecular Clouds Kloster Seeon, Germany 16/06/2011 VLA/ANGST The ANGST HST Treasury Project allowed
More informationA Comparison of an HPGe-based and NaI-based Radionuclide Identifier (RID) for Radioactive Materials
Illicit Trafficking, Sub/cross-national threats, Poster presentation A Comparison of an HPGe-based and NaI-based Radionuclide Identifier (RID) for Radioactive Materials Ronald M. Keyser, Timothy R. Twomey,
More informationThe Main Point. Lecture #34: Solar System Origin II. Chemical Condensation ( Lewis ) Model. How did the solar system form? Reading: Chapter 8.
Lecture #34: Solar System Origin II How did the solar system form? Chemical Condensation ("Lewis") Model. Formation of the Terrestrial Planets. Formation of the Giant Planets. Planetary Evolution. Reading:
More informationChapter 6 Atmospheric Aerosol and Cloud Processes Spring 2015 Cloud Physics Initiation and development of cloud droplets Special interest: Explain how droplet formation results in rain in approximately
More informationSecondary Ion Mass Spectrometry
Secondary Ion Mass Spectrometry A PRACTICAL HANDBOOK FOR DEPTH PROFILING AND BULK IMPURITY ANALYSIS R. G. Wilson Hughes Research Laboratories Malibu, California F. A. Stevie AT&T Bell Laboratories Allentown,
More informationDinamica del Gas nelle Galassie II. Star formation
Dinamica del Gas nelle Galassie II. Star formation Overview on ISM Molecular clouds: composition and properties. Plasmas Charge neutrality, infinite conductivity; Field freezing; Euler equation with magnetic
More informationLesson 3: Isothermal Hydrostatic Spheres. B68: a self-gravitating stable cloud. Hydrostatic self-gravitating spheres. P = "kt 2.
Lesson 3: Isothermal Hydrostatic Spheres B68: a self-gravitating stable cloud Bok Globule Relatively isolated, hence not many external disturbances Though not main mode of star formation, their isolation
More informationThe soot and scale problems
Dr. Albrecht Kaupp Page 1 The soot and scale problems Issue Soot and scale do not only increase energy consumption but are as well a major cause of tube failure. Learning Objectives Understanding the implications
More informationHomework #4 Solutions ASTR100: Introduction to Astronomy Fall 2009: Dr. Stacy McGaugh
Homework #4 Solutions ASTR100: Introduction to Astronomy Fall 2009: Dr. Stacy McGaugh Chapter 5: #50 Hotter Sun: Suppose the surface temperature of the Sun were about 12,000K, rather than 6000K. a. How
More informationChemical Bonds. Chemical Bonds. The Nature of Molecules. Energy and Metabolism < < Covalent bonds form when atoms share 2 or more valence electrons.
The Nature of Molecules Chapter 2 Energy and Metabolism Chapter 6 Chemical Bonds Molecules are groups of atoms held together in a stable association. Compounds are molecules containing more than one type
More informationMBA Lattice Upgrade: New Opportunities for In-situ High Energy (30 kev 90 kev) X-ray Structural Analyses
MBA Lattice Upgrade: New Opportunities for In-situ High Energy (30 kev 90 kev) X-ray Structural Analyses David Tiede Chemical Sciences and Engineering Division Argonne National Laboratory Workshop on New
More informationOverview. What is EMR? Electromagnetic Radiation (EMR) LA502 Special Studies Remote Sensing
LA502 Special Studies Remote Sensing Electromagnetic Radiation (EMR) Dr. Ragab Khalil Department of Landscape Architecture Faculty of Environmental Design King AbdulAziz University Room 103 Overview What
More informationClouds and the Energy Cycle
August 1999 NF-207 The Earth Science Enterprise Series These articles discuss Earth's many dynamic processes and their interactions Clouds and the Energy Cycle he study of clouds, where they occur, and
More informationModeling Gas-Grain Chemistry in Dark Cloud Conditions
Modeling Gas-Grain Chemistry in Dark Cloud Conditions Dissertation zur Erlangung des Doktorgrades (Dr. rer. nat.) der Mathematisch-Naturwissenschaftlichen Fakultät der Rheinischen Friedrich-Wilhelms-Universität
More information............... [2] At the time of purchase of a Strontium-90 source, the activity is 3.7 10 6 Bq.
1 Strontium-90 decays with the emission of a β-particle to form Yttrium-90. The reaction is represented by the equation 90 38 The decay constant is 0.025 year 1. 90 39 0 1 Sr Y + e + 0.55 MeV. (a) Suggest,
More informationSSO Transmission Grating Spectrograph (TGS) User s Guide
SSO Transmission Grating Spectrograph (TGS) User s Guide The Rigel TGS User s Guide available online explains how a transmission grating spectrograph (TGS) works and how efficient they are. Please refer
More informationPhysical Self-Calibration of X-ray and SZ Surveys
Physical Self-Calibration of X-ray and SZ Surveys Greg L. Bryan, Zoltan Haiman (Columbia University) and Joshua D. Younger (CfA) 1. Cluster Surveys and Self-Calibration Clusters of galaxies form at the
More informationINFRARED MONITORING OF 110 GHz GYROTRON WINDOWS AT DIII D
GA A23981 INFRARED MONITORING OF 110 GHz GYROTRON WINDOWS AT DIII D by Y. GORELOV, J. LOHR, R.W. CALLIS, and D. PONCE MAY 2002 DISCLAIMER This report was prepared as an account of work sponsored by an
More informationAccurate calibration of on-line Time of Flight Mass Spectrometer (TOF-MS) for high molecular weight combustion product analysis
Accurate calibration of on-line Time of Flight Mass Spectrometer (TOF-MS) for high molecular weight combustion product analysis B. Apicella*, M. Passaro**, X. Wang***, N. Spinelli**** mariadellarcopassaro@gmail.com
More informationUsed to determine relative location of atoms within a molecule Most helpful spectroscopic technique in organic chemistry Related to MRI in medicine
Structure Determination: Nuclear Magnetic Resonance CHEM 241 UNIT 5C 1 The Use of NMR Spectroscopy Used to determine relative location of atoms within a molecule Most helpful spectroscopic technique in
More informationIn studying the Milky Way, we have a classic problem of not being able to see the forest for the trees.
In studying the Milky Way, we have a classic problem of not being able to see the forest for the trees. A panoramic painting of the Milky Way as seen from Earth, done by Knut Lundmark in the 1940 s. The
More informationWJP, PHY381 (2015) Wabash Journal of Physics v4.3, p.1. Cloud Chamber. R.C. Dennis, Tuan Le, M.J. Madsen, and J. Brown
WJP, PHY381 (2015) Wabash Journal of Physics v4.3, p.1 Cloud Chamber R.C. Dennis, Tuan Le, M.J. Madsen, and J. Brown Department of Physics, Wabash College, Crawfordsville, IN 47933 (Dated: May 7, 2015)
More informationHow To Understand The Physics Of Electromagnetic Radiation
Ay 122 - Fall 2004 Electromagnetic Radiation And Its Interactions With Matter (This version has many of the figures missing, in order to keep the pdf file reasonably small) Radiation Processes: An Overview
More informationThe Evolution of GMCs in Global Galaxy Simulations
The Evolution of GMCs in Global Galaxy Simulations image from Britton Smith Elizabeth Tasker (CITA NF @ McMaster) Jonathan Tan (U. Florida) Simulation properties We use the AMR code, Enzo, to model a 3D
More informationNMR Chemical Shifts of Common Laboratory Solvents as Trace Impurities
7512 J. Org. Chem. 1997, 62, 7512-7515 NMR Chemical Shifts of Common Laboratory Solvents as Trace Impurities Hugo E. Gottlieb,* Vadim Kotlyar, and Abraham Nudelman* Department of Chemistry, Bar-Ilan University,
More informationPassive Remote Sensing of Clouds from Airborne Platforms
Passive Remote Sensing of Clouds from Airborne Platforms Why airborne measurements? My instrument: the Solar Spectral Flux Radiometer (SSFR) Some spectrometry/radiometry basics How can we infer cloud properties
More informationIt has long been a goal to achieve higher spatial resolution in optical imaging and
Nano-optical Imaging using Scattering Scanning Near-field Optical Microscopy Fehmi Yasin, Advisor: Dr. Markus Raschke, Post-doc: Dr. Gregory Andreev, Graduate Student: Benjamin Pollard Department of Physics,
More information1. A wire carries 15 A. You form the wire into a single-turn circular loop with magnetic field 80 µ T at the loop center. What is the loop radius?
CHAPTER 3 SOURCES O THE MAGNETC ELD 1. A wire carries 15 A. You form the wire into a single-turn circular loop with magnetic field 8 µ T at the loop center. What is the loop radius? Equation 3-3, with
More informationFrost Damage of Roof Tiles in Relatively Warm Areas in Japan
Frost Damage of Roof Tiles in Relatively Warm Areas in Japan Influence of Surface Finish on Water Penetration Chiemi IBA Hokkaido Research Organization, Japan Shuichi HOKOI Kyoto University, Japan INTRODUCTION
More information1 The water molecule and hydrogen bonds in water
The Physics and Chemistry of Water 1 The water molecule and hydrogen bonds in water Stoichiometric composition H 2 O the average lifetime of a molecule is 1 ms due to proton exchange (catalysed by acids
More informationThe Birth of the Universe Newcomer Academy High School Visualization One
The Birth of the Universe Newcomer Academy High School Visualization One Chapter Topic Key Points of Discussion Notes & Vocabulary 1 Birth of The Big Bang Theory Activity 4A the How and when did the universe
More informationPdr Reflection of the FUV radiation field
Properties of the Molecular Gas in Low Metallicity Environments Dissertation zur Erlangung des Doktorgrades (Dr. rer. nat.) der Mathematisch Naturwissenschaftlichen Fakultät der Rheinischen Friedrich Wilhelms
More informationThe Greenhouse Effect. Lan Ma Global Warming: Problems & Solutions 17 September, 2007
The Greenhouse Effect Lan Ma Global Warming: Problems & Solutions 17 September, 2007 What to cover today: How do we calculate the Earth s surface temperature? What makes a gas a greenhouse gas and how
More informationHVAC air curtains. Type InduAir
Air Conditioning Cooling Heating Ventilation HVAC air curtains Type InduAir The Energy Saving air curtain for Industrial Applications InduAir The solid, self-supporting housing of the energy saving air
More informationStar Formation in the Large Magellanic Cloud: Tracing an Evolution of Giant Molecular Clouds
Star Formation in the Large Magellanic Cloud: Tracing an Evolution of Giant Molecular Clouds Toshikazu Onishi Osaka Prefecture University Yasuo Fukui; Akiko Kawamura; Norikazu Mizuno; Tetsuhiro Minamidani;
More informationAbsorption by atmospheric gases in the IR, visible and UV spectral regions.
Lecture 6. Absorption by atmospheric gases in the IR, visible and UV spectral regions. Objectives: 1. Gaseous absorption in thermal IR. 2. Gaseous absorption in the visible and near infrared. 3. Gaseous
More informationCovalent Conjugation to Cytodiagnostics Carboxylated Gold Nanoparticles Tech Note #105
Covalent Conjugation to Cytodiagnostics Carboxylated Gold Nanoparticles Tech Note #105 Background Gold nanoparticle conjugates have been widely used in biological research and biosensing applications.
More informationPROTON NUCLEAR MAGNETIC RESONANCE SPECTROSCOPY (H-NMR)
PROTON NUCLEAR MAGNETIC RESONANCE SPECTROSCOPY (H-NMR) WHAT IS H-NMR SPECTROSCOPY? References: Bruice 14.1, 14.2 Introduction NMR or nuclear magnetic resonance spectroscopy is a technique used to determine
More informationParticulate matter sources in Helsinki area and effects on air quality - an overview
Particulate matter sources in Helsinki area and effects on air quality - an overview Risto Hillamo 1, Topi Rönkkö 2 and Liisa Pirjola 3 1 Research and Development, Finnish Meteorological Institute 2 Department
More informationDISCLAIMER. This document was prepared as an account of work sponsored by an agency of the United States
DISCLAIMER This document was prepared as an account of work sponsored by an agency of the United States Government. Neither the United States Government nor the University of California nor any of their
More informationINTI COLLEGE MALAYSIA A? LEVEL PROGRAMME CHM 111: CHEMISTRY MOCK EXAMINATION: DECEMBER 2000 SESSION. 37 74 20 40 60 80 m/e
CHM111(M)/Page 1 of 5 INTI COLLEGE MALAYSIA A? LEVEL PROGRAMME CHM 111: CHEMISTRY MOCK EXAMINATION: DECEMBER 2000 SESSION SECTION A Answer ALL EIGHT questions. (52 marks) 1. The following is the mass spectrum
More informationL. Yu et al. Correspondence to: Q. Zhang (dkwzhang@ucdavis.edu)
Supplement of Atmos. Chem. Phys. Discuss., 5, 967 974, 5 http://www.atmos-chem-phys-discuss.net/5/967/5/ doi:.594/acpd-5-967-5-supplement Author(s) 5. CC Attribution. License. Supplement of Molecular transformations
More informationPrinciples of Ion Implant
Principles of Ion Implant Generation of ions dopant gas containing desired species BF 3, B 2 H 6, PH 3, AsH 3, AsF 5 plasma provides positive ions (B 11 ) +, BF 2+, (P 31 ) +, (P 31 ) ++ Ion Extraction
More informationASTRONOMY AND ASTROPHYSICS. Deep search for CO emission in the Low Surface Brightness galaxy Malin 1. J. Braine 1, F. Herpin 1,2, and S.J.E.
Astron. Astrophys. 358, 494 498 (2000) Deep search for CO emission in the Low Surface Brightness galaxy Malin 1 ASTRONOMY AND ASTROPHYSICS J. Braine 1, F. Herpin 1,2, and S.J.E. Radford 3 1 Observatoire
More informationSupporting Information
Supporting Information Wiley-VCH 2007 69451 Weinheim, Germany Methanol Behavior in Direct Methanol Fuel Cells Younkee Paik, Seong-Soo Kim, and Oc Hee Han * Experimental Section Preparation of MEA: Standard
More informationLecture 10 Formation of the Solar System January 6c, 2014
1 Lecture 10 Formation of the Solar System January 6c, 2014 2 Orbits of the Planets 3 Clues for the Formation of the SS All planets orbit in roughly the same plane about the Sun. All planets orbit in the
More informationAN EFFECT OF GRID QUALITY ON THE RESULTS OF NUMERICAL SIMULATIONS OF THE FLUID FLOW FIELD IN AN AGITATED VESSEL
14 th European Conference on Mixing Warszawa, 10-13 September 2012 AN EFFECT OF GRID QUALITY ON THE RESULTS OF NUMERICAL SIMULATIONS OF THE FLUID FLOW FIELD IN AN AGITATED VESSEL Joanna Karcz, Lukasz Kacperski
More informationarxiv:0911.3922v1 [astro-ph.ga] 19 Nov 2009
The Initial Conditions of Clustered Star Formation II: N 2 H + Observations of the Ophiuchus B Core R. K. Friesen 1,2 arxiv:0911.3922v1 [astro-ph.ga] 19 Nov 2009 rachel.friesen@nrc-cnrc.gc.ca J. Di Francesco
More information1. Introduction 2. The H 2 Molecule 3. The CO Molecule 4. Summary. 1. Introduction
Lecture 19. The H 2 and CO Molecules 1. Introduction 2. The H 2 Molecule 3. The CO Molecule 4. Summary References Stahler & Palla, The Formation of Stars, Secs. 5.2-3 Shull & Beckwith, ARAA 20 163 1982
More informationChem 106 Thursday Feb. 3, 2011
Chem 106 Thursday Feb. 3, 2011 Chapter 13: -The Chemistry of Solids -Phase Diagrams - (no Born-Haber cycle) 2/3/2011 1 Approx surface area (Å 2 ) 253 258 Which C 5 H 12 alkane do you think has the highest
More informationThe CGM around Dwarf Galaxies
The CGM around Dwarf Galaxies Rongmon Bordoloi STScI + the COS-Halos Team What is the CGM? Shen et al. 212 jectedcolumndensityinacubeof5(proper)kpc Diffuse gas, including metals and dust, o2en on extending
More information2. Room temperature: C. Kelvin. 2. Room temperature:
Temperature I. Temperature is the quantity that tells how hot or cold something is compared with a standard A. Temperature is directly proportional to the average kinetic energy of molecular translational
More informationA Star and Gas Surface Density Correlation within Nearby Molecular Clouds
A Star and Gas Surface Density Correlation within Nearby Molecular Clouds Rob Gutermuth Five College Astronomy Dept. Fellow in Research & Teaching Smith College & UMass Amherst MonR2 Giant Molecular Cloud
More informationTitan: The Solar System s Abiotic Petroleum Factory
Titan: The Solar System s Abiotic Petroleum Factory J. Hunter Waite, Ph.D. Institute Scientist Space Science & Engineering Division Southwest Research Institute Titan: The Solar System s Abiotic Petroleum
More informationCathode Ray Tube. Introduction. Functional principle
Introduction The Cathode Ray Tube or Braun s Tube was invented by the German physicist Karl Ferdinand Braun in 897 and is today used in computer monitors, TV sets and oscilloscope tubes. The path of the
More informationThe illustrations in this manual may differ from the product you are using.
The illustrations in this manual may differ from the product you are using. 1 1 2 1 2 3 1 4 1 5 6 7 8 9 Youkei No.4 (105 mm 235 mm) (Envelope Y401 for Canon LBP/recommended) * You cannot use envelopes
More informationChemical Sputtering. von Kohlenstoff durch Wasserstoff. W. Jacob
Chemical Sputtering von Kohlenstoff durch Wasserstoff W. Jacob Centre for Interdisciplinary Plasma Science Max-Planck-Institut für Plasmaphysik, 85748 Garching Content: Definitions: Chemical erosion, physical
More informationCOOKBOOK. for. Aristarchos Transient Spectrometer (ATS)
NATIONAL OBSERVATORY OF ATHENS Institute for Astronomy, Astrophysics, Space Applications and Remote Sensing HELMOS OBSERVATORY COOKBOOK for Aristarchos Transient Spectrometer (ATS) P. Boumis, J. Meaburn,
More informationSupporting Information. The G-triplex DNA could function as a new variety of DNA peroxidase
Supporting Information The G-triplex DNA could function as a new variety of DNA peroxidase Shaoru Wang +, Boshi Fu +, Shuang Peng, Xiaoe Zhang, Tian Tian*, Xiang Zhou* College of Chemistry and Molecular
More informationWhich month has larger and smaller day time?
ACTIVITY-1 Which month has larger and smaller day time? Problem: Which month has larger and smaller day time? Aim: Finding out which month has larger and smaller duration of day in the Year 2006. Format
More informationPlanck Early Results: New light on Anomalous Microwave Emission from Spinning Dust Grains
Planck Early Results: New light on Anomalous Microwave Emission from Spinning Dust Grains Perseus in the optical Clive Dickinson Jodrell Bank Centre for Astrophysics (University of Manchester) On behalf
More informationALMA Newsletter. ALMA In-depth. How Will ALMA Make Images? April 2010
How Will ALMA Make Images? Credit: ALMA (ESO / NAOJ / NRAO), Cynthia Collao (ALMA). The invention of the optical telescope by Galileo 400 years ago marked the beginning of modern astronomy. Galileo used
More informationSpecifying Plasma Deposited Hard Coated Optical Thin Film Filters. Alluxa Engineering Staff
Specifying Plasma Deposited Hard Coated Optical Thin Film Filters. Alluxa Engineering Staff December 2012 Specifying Advanced Plasma Deposited Hard Coated Optical Bandpass and Dichroic Filters. Introduction
More informationAnna Serdyuchenko, Victor Gorshelev, Mark Weber John P. Burrows University of Bremen, Institute for Environmental Physics
Anna Serdyuchenko, Victor Gorshelev, Mark Weber John P. Burrows University of Bremen, Institute for Environmental Physics 3-5 June 2013 ACSO meeting WMO Geneva, Switzerland 1 Graphics: DLR-IMF 3-5 June
More informationDemonstration of the Applicability of 3D Slicer to Astronomical Data Using
Demonstration of the Applicability of 3D Slicer to Astronomical Data Using 13 CO and C 18 O Observations of IC 348 Michelle A. Borkin 1, Naomi A. Ridge 2, Alyssa A. Goodman 2, & Michael Halle 3 1 Harvard
More informationNatural Convection. Buoyancy force
Natural Convection In natural convection, the fluid motion occurs by natural means such as buoyancy. Since the fluid velocity associated with natural convection is relatively low, the heat transfer coefficient
More informationStellar Evolution: a Journey through the H-R Diagram
Stellar Evolution: a Journey through the H-R Diagram Mike Montgomery 21 Apr, 2001 0-0 The Herztsprung-Russell Diagram (HRD) was independently invented by Herztsprung (1911) and Russell (1913) They plotted
More informationATOMS. Multiple Choice Questions
Chapter 3 ATOMS AND MOLECULES Multiple Choice Questions 1. Which of the following correctly represents 360 g of water? (i) 2 moles of H 2 0 (ii) 20 moles of water (iii) 6.022 10 23 molecules of water (iv)
More informationTechnical Information
Technical Information TI No. WL 80-63 E April 2001 Rolling Bearing Diagnosis with the FAG Bearing Analyser Rolling Bearings State-Of-The-Art, Condition-Related Monitoring of Plants and Machines Unforeseen
More informationRaman spectroscopy Lecture
Raman spectroscopy Lecture Licentiate course in measurement science and technology Spring 2008 10.04.2008 Antti Kivioja Contents - Introduction - What is Raman spectroscopy? - The theory of Raman spectroscopy
More informationAP CHEMISTRY 2013 SCORING GUIDELINES
AP CHEMISTRY 2013 SCORING GUIDELINES Question 4 (15 points) For each of the following three reactions, write a balanced equation for the reaction in part (i) and answer the question about the reaction
More informationInfrared Spectroscopy 紅 外 線 光 譜 儀
Infrared Spectroscopy 紅 外 線 光 譜 儀 Introduction Spectroscopy is an analytical technique which helps determine structure. It destroys little or no sample (nondestructive method). The amount of light absorbed
More informationAdaptive feature selection for rolling bearing condition monitoring
Adaptive feature selection for rolling bearing condition monitoring Stefan Goreczka and Jens Strackeljan Otto-von-Guericke-Universität Magdeburg, Fakultät für Maschinenbau Institut für Mechanik, Universitätsplatz,
More informationChapter 3 Student Reading
Chapter 3 Student Reading If you hold a solid piece of lead or iron in your hand, it feels heavy for its size. If you hold the same size piece of balsa wood or plastic, it feels light for its size. The
More informationOrder of Filling Subshells
Bonding: General Concepts Ionic Bonds Sections 13.2-13.6 Covalent Bonds Section 13.7 Covalent Bond Energy & Chemical Reactions Section 13.8-13.9 Lewis Structures Sections 13.10-13.12 VSEPR Theory Section
More informationBe Stars. By Carla Morton
Be Stars By Carla Morton Index 1. Stars 2. Spectral types 3. B Stars 4. Be stars 5. Bibliography How stars are formed Stars are composed of gas Hydrogen is the main component of stars. Stars are formed
More informationTotal radiative heating/cooling rates.
Lecture. Total radiative heating/cooling rates. Objectives:. Solar heating rates.. Total radiative heating/cooling rates in a cloudy atmosphere.. Total radiative heating/cooling rates in different aerosol-laden
More informationThe atmospheres of different planets
The atmospheres of different planets Thomas Baron October 13, 2006 1 Contents 1 Introduction 3 2 The atmosphere of the Earth 3 2.1 Description and Composition.................... 3 2.2 Discussion...............................
More informationNuclear Magnetic Resonance notes
Reminder: These notes are meant to supplement, not replace, the laboratory manual. Nuclear Magnetic Resonance notes Nuclear Magnetic Resonance (NMR) is a spectrometric technique which provides information
More informationDO PHYSICS ONLINE FROM QUANTA TO QUARKS QUANTUM (WAVE) MECHANICS
DO PHYSICS ONLINE FROM QUANTA TO QUARKS QUANTUM (WAVE) MECHANICS Quantum Mechanics or wave mechanics is the best mathematical theory used today to describe and predict the behaviour of particles and waves.
More information