Annual Report 2003
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Metallicities of the Β Cephei Stars from Low-Resolution Ultraviolet Spectra
A&A 433, 659–669 (2005) Astronomy DOI: 10.1051/0004-6361:20040396 & c ESO 2005 Astrophysics Metallicities of the β Cephei stars from low-resolution ultraviolet spectra E. Niemczura and J. Daszynska-Daszkiewicz´ Astronomical Institute, Wrocław University, ul. Kopernika 11, 51-622 Wrocław, Poland e-mail: [email protected] Received 5 March 2004 / Accepted 22 November 2004 Abstract. We derive basic stellar parameters (angular diameters, effective temperatures, metallicities) and interstellar reddening for all β Cephei stars observed during the IUE satellite mission, including those belonging to three open clusters. The parameters are derived by means of an algorithmic procedure of fitting theoretical flux distributions to the low-resolution IUE spectra and ground-based spectrophotometric observations. Since the metallicity has a special importance for pulsating B-type stars, we focus our attention in particular on this parameter. Key words. stars: early-type – stars: abundances – stars: variables: general 1. Introduction In this paper we analyze the IUE (International Ultraviolet Explorer) data combined with ground-based spectrophotomet- β Cephei variables are a well-known group of early B-type ric observations of β Cephei stars. The ultraviolet (UV) part pulsating stars. Their pulsations are driven by the classical of the spectra of main-sequence B-type stars is very rich in κ-mechanism, operating in the layer of the metal opacity bump lines of the iron-group elements. Because the greatest amount ≈ × 5 at T 2 10 K caused by the large number of absorption of energy for these objects is emitted in the spectral region be- lines of the iron-group elements. -
Wynyard Planetarium & Observatory a Autumn Observing Notes
Wynyard Planetarium & Observatory A Autumn Observing Notes Wynyard Planetarium & Observatory PUBLIC OBSERVING – Autumn Tour of the Sky with the Naked Eye CASSIOPEIA Look for the ‘W’ 4 shape 3 Polaris URSA MINOR Notice how the constellations swing around Polaris during the night Pherkad Kochab Is Kochab orange compared 2 to Polaris? Pointers Is Dubhe Dubhe yellowish compared to Merak? 1 Merak THE PLOUGH Figure 1: Sketch of the northern sky in autumn. © Rob Peeling, CaDAS, 2007 version 1.2 Wynyard Planetarium & Observatory PUBLIC OBSERVING – Autumn North 1. On leaving the planetarium, turn around and look northwards over the roof of the building. Close to the horizon is a group of stars like the outline of a saucepan with the handle stretching to your left. This is the Plough (also called the Big Dipper) and is part of the constellation Ursa Major, the Great Bear. The two right-hand stars are called the Pointers. Can you tell that the higher of the two, Dubhe is slightly yellowish compared to the lower, Merak? Check with binoculars. Not all stars are white. The colour shows that Dubhe is cooler than Merak in the same way that red-hot is cooler than white- hot. 2. Use the Pointers to guide you upwards to the next bright star. This is Polaris, the Pole (or North) Star. Note that it is not the brightest star in the sky, a common misconception. Below and to the left are two prominent but fainter stars. These are Kochab and Pherkad, the Guardians of the Pole. Look carefully and you will notice that Kochab is slightly orange when compared to Polaris. -
物理雙月刊29-3 621-772.Pdf
ᒳृݧ ʳ ౨ᄭઝݾറᙀ ᚮࣔᏕ/֮ ΔࢨუԵᛵᇞݺଚشଶಬߨጿጿլឰऱਞ ၦऱࠌ ౨ᄭऱ࣠Δኙ٤شॸΔ᠏ณհၴԾࠩԱքΕԮִ መ৫ࠌ ഏᎾၴऱڇऱᐙګԳพஒऱ ᛩቼࢬທח᥆࣍ङऱֲΔ עء۶ΔլោᥦԫՀڕټᚰۖࠐΖ ඈچᑷԫंंլឰ Δᑷ รԼᒧറ֮ΚψൕഏᎾᛩቼਐᑇࡌ௧ᛩ៥ऱ ऱ࿇ሽ౨ᄭऱᛘΔ ֗ IEA อૠװထԫैཀհլ݈ ωΔᇠᒧ֮ີტխᘋՕᖂ܉ऱՕհխΔᨃԳ ։ᗺ៥࣍ ᤚຑ़Εຑ௧ຟआᤴ ढߓ୪ւࣳඒ࣍ඒᖂઔߒ խࢼ़ݺଚᐷᐊΖڦۍऱ ᎩհᎾΔڼԱΖՈࠌଖ ᆖᛎࡉഏԺऱ࿇୶זᆏᆏՂ چሽլឰشڞऱ ᎅ࠷ެ࣍౨ᄭױሽ ፖᑓΔ༓شڇΔኚ໌ΖྥۖΔ֒ Δޡݾऱၞشࠡሎ֗شழΔݺଚՈՕ ऱࠌٵཚऱ ᎅਢԫഏᆖᛎ࿇୶ऱױCO2 ऱඈ࣋ၦࡉᄵயᚨ ౨ᄭ ٺΔ౨ᄭᤜᠲኙ࣍ڼڂऱ༞֏ΔထኔఎՀԱլ֟լߜ ೯ԺΖ ࡳࢤެڶᏆऱ࿇୶ࠠٺڇᄊ֏ ഏچຒףԱګऱધᙕΔՈ ߪᣂএࠩԫषᄎՕฒऱ壂ઘࡉֲൄढ֊ޓயᚨऱං֫հԫΖ ऱᐙΔ ฒاڇवኙ࣍ Ꮭऱं೯ΖᅝഏᎾईᏝՂཆΔഏփढᏝঁஓஓױݺଚࠆ࠹ԫաऱ堚ළፖঁ൸հᎾΔڇ ՂይΖچΔ ऱৼᜢխᆥྤݲᐫᇷᄭᤖ៲ຆΔ౨ᄭ༓٤ᑇٛᘸၞՑऱྥ֚ 9 ڣ ࣍ 2005ޓࠐΔईᏝᆏᆏ֒Δڣၦথբ २༓شࢬऱؓ݁ሽၦࡉ౨ᄭࠌڣޢԳޢݺଚ ද࣍ US$70 ऱ໌ޢࠐऱᖵᄅΔሒڣۍሽ ִٝડధڇ౨ᄭΕڇऱছૄΜૉ൞უڇټਢඈ ᄭ۞ᖏञࡉైڂຝ։ڶᄅધᙕΖईᏝऱं೯ឈ ᚮࣔᏕ ౨ᄭفՂ֏چլ؆ਢڂԫ܀ਙएࠃٙΔ 堚ဎՕᖂढߓمഏ ڶईΕ֚ྥࡉᅁ౨ᄭᗏற)ऱᤖ៲ၦึߒفऑਐ) E-mail: [email protected] ࢤΔૉشऱ౨ᄭࠌڶૻΖറ୮ေ۷ૉᖕԳᣊ Ϯ621Ϯʳ քִʳڣ ˊ˃˃˅ʻ֥࠴Կཚʼʳעढᠨִ ᒳृݧ ༚ྼऱႨΖᅝᓫᓵᇠ֘ுΛࢨਢᇠᖑுΛംᠲڶۖ ࠩބயऱᆏ౨ֱூΔࢨլᕣݶ༈ڶإటנ༼౨آᙈᙈ ᇞு౨ᗏறऱ፹ທመچհছΔषᄎՕฒᚨᇠ٣堚ᄑ ڶՂೈᅁᇷᄭࡸچ౨ᄭऱᇩΔঞזࠠயհཙ ؆ਜ਼ழऱۆுᘿ୴֗אΔ܂࿓ࡉு౨࿇ሽऱՠ فईࡉ֚ྥ֏فڕהऱᤖ៲ၦ؆Δࠡ׳ؐڣ 200 ࢤড়ᨠऱኪ৫אթ౨ڼڕୌࠄΔڶՂऱ ᥨൻਜࠩࢍאڣ ౨ྤऄ֭ᐶመ 50ױၦቃ۷ژᗏறऱᚏ ཚءΔڼڂᖗΖހᒔऱإԫנு౨࿇ሽشࠌܡၦΖ ਢޣ౨ᄭ᜔Ꮑ ሽֆுԿᐗૠቤิ९ದ໑Փऱᑷ֧֨ᗏ ܑຘመف᠏ངயለհႚอ֏܅ءګΔᆖᛎۖྥ ሽֆு౨࿇ሽኔ೭ᆖ᧭ऱڣڍڶࠩԱٍࠠބऱሽ౨ Δشऴ൷ࠌאԫՕฒګ᠏ངڇΔشறऱࠌ ،ݺଚ֮റ૪ψࢢسࢨᑷ౨ऱመ࿓խΔᄎ ு֨ᛜሎᓰᓰ९׆ᐚᆠ٣(شԺ࿇ሽ)Ε೯౨(ሎᙁ־อጠ) ॺൄ᧩࣐ᚩऱאԱᇞ،--ு౨࿇ሽᓫωΔᇠ֮ڕլ ۆᎨॸΔᖄીᣤૹऱᛩቼګඈ࣋Օၦऱᄵ᧯ࡉݮ ຝٺᎅࣔԱு౨࿇ሽऱچᦰृ堚ᄑڗऱؓ݁ᄵ৫ 壄֮چࡉֲᣤૹऱᄵயᚨΔၞۖᖄી ኪؓᘝ ੌ࿓ࡉுᗏறՄऱ፹ທመ࿓Δਢԫᒧॺൄଖԫᦰऱسऱڶऱ۞ྥᛩቼࡉچኙۖڂດዬՂ֒Ζ ኪᛩቼ૿ ֮ີΖسऱچऱᣤૹᓢᚰΔࠌڃனױլګؘലທ ٤ᤜᠲǵഏᎾईᏝࡺլڜईفᜯ؎ՕऱਗᖏΖ ࠹ࠩ٤ ՂഏᎾၴᒤᄵ᧯ඈ࣋྇ၦࢭᘭհᛩঅֆףࡉଢऱ᧢ᔢࢬທ ՀΔ᧢ޏኙᛩቼऱشᣂ౨ᄭሎڶ ڂᛩঅრᢝይ֗אඔ೯ΔڤإऱᐙຍଡૹᤜᠲΔݺଚܑࡡᓮՠᄐݾઔߒ પψࠇຟᤜࡳωګ ԳᣊؘߨհሁΖ۶ᘯګ౨ᄭسᡖᐚ ైऱᓢᚰՀΔං೯٦ۂ(Հ១ጠՠઔೃ౨ᛩࢬא)ೃ౨ᄭፖᛩቼઔߒࢬ ౨ᄭ࿇ሽωٍᆖسรքᒧറ֮ψ٦עء౨ᄭΛس٦ -
Astronomy 2008 Index
Astronomy Magazine Article Title Index 10 rising stars of astronomy, 8:60–8:63 1.5 million galaxies revealed, 3:41–3:43 185 million years before the dinosaurs’ demise, did an asteroid nearly end life on Earth?, 4:34–4:39 A Aligned aurorae, 8:27 All about the Veil Nebula, 6:56–6:61 Amateur astronomy’s greatest generation, 8:68–8:71 Amateurs see fireballs from U.S. satellite kill, 7:24 Another Earth, 6:13 Another super-Earth discovered, 9:21 Antares gang, The, 7:18 Antimatter traced, 5:23 Are big-planet systems uncommon?, 10:23 Are super-sized Earths the new frontier?, 11:26–11:31 Are these space rocks from Mercury?, 11:32–11:37 Are we done yet?, 4:14 Are we looking for life in the right places?, 7:28–7:33 Ask the aliens, 3:12 Asteroid sleuths find the dino killer, 1:20 Astro-humiliation, 10:14 Astroimaging over ancient Greece, 12:64–12:69 Astronaut rescue rocket revs up, 11:22 Astronomers spy a giant particle accelerator in the sky, 5:21 Astronomers unearth a star’s death secrets, 10:18 Astronomers witness alien star flip-out, 6:27 Astronomy magazine’s first 35 years, 8:supplement Astronomy’s guide to Go-to telescopes, 10:supplement Auroral storm trigger confirmed, 11:18 B Backstage at Astronomy, 8:76–8:82 Basking in the Sun, 5:16 Biggest planet’s 5 deepest mysteries, The, 1:38–1:43 Binary pulsar test affirms relativity, 10:21 Binocular Telescope snaps first image, 6:21 Black hole sets a record, 2:20 Black holes wind up galaxy arms, 9:19 Brightest starburst galaxy discovered, 12:23 C Calling all space probes, 10:64–10:65 Calling on Cassiopeia, 11:76 Canada to launch new asteroid hunter, 11:19 Canada’s handy robot, 1:24 Cannibal next door, The, 3:38 Capture images of our local star, 4:66–4:67 Cassini confirms Titan lakes, 12:27 Cassini scopes Saturn’s two-toned moon, 1:25 Cassini “tastes” Enceladus’ plumes, 7:26 Cepheus’ fall delights, 10:85 Choose the dome that’s right for you, 5:70–5:71 Clearing the air about seeing vs. -
October 2006
OCTOBER 2 0 0 6 �������������� http://www.universetoday.com �������������� TAMMY PLOTNER WITH JEFF BARBOUR 283 SUNDAY, OCTOBER 1 In 1897, the world’s largest refractor (40”) debuted at the University of Chica- go’s Yerkes Observatory. Also today in 1958, NASA was established by an act of Congress. More? In 1962, the 300-foot radio telescope of the National Ra- dio Astronomy Observatory (NRAO) went live at Green Bank, West Virginia. It held place as the world’s second largest radio scope until it collapsed in 1988. Tonight let’s visit with an old lunar favorite. Easily seen in binoculars, the hexagonal walled plain of Albategnius ap- pears near the terminator about one-third the way north of the south limb. Look north of Albategnius for even larger and more ancient Hipparchus giving an almost “figure 8” view in binoculars. Between Hipparchus and Albategnius to the east are mid-sized craters Halley and Hind. Note the curious ALBATEGNIUS AND HIPPARCHUS ON THE relationship between impact crater Klein on Albategnius’ southwestern wall and TERMINATOR CREDIT: ROGER WARNER that of crater Horrocks on the northeastern wall of Hipparchus. Now let’s power up and “crater hop”... Just northwest of Hipparchus’ wall are the beginnings of the Sinus Medii area. Look for the deep imprint of Seeliger - named for a Dutch astronomer. Due north of Hipparchus is Rhaeticus, and here’s where things really get interesting. If the terminator has progressed far enough, you might spot tiny Blagg and Bruce to its west, the rough location of the Surveyor 4 and Surveyor 6 landing area. -
The Impact of Giant Stellar Outflows on Molecular Clouds
The Impact of Giant Stellar Outflows on Molecular Clouds A thesis presented by H´ector G. Arce Nazario to The Department of Astronomy in partial fulfillment of the requirements for the degree of Doctor of Philosophy in the subject of Astronomy Harvard University Cambridge, Massachusetts October, 2001 c 2001, by H´ector G. Arce Nazario All Rights Reserved ABSTRACT Thesis Advisor: Alyssa A. Goodman Thesis by: H´ector G. Arce Nazario We use new millimeter wavelength observations to reveal the important effects that giant (parsec-scale) outflows from young stars have on their surroundings. We find that giant outflows have the potential to disrupt their host cloud, and/or drive turbulence there. In addition, our study confirms that episodicity and a time-varying ejection axis are common characteristics of giant outflows. We carried out our study by mapping, in great detail, the surrounding molecular gas and parent cloud of two giant Herbig-Haro (HH) flows; HH 300 and HH 315. Our study shows that these giant HH flows have been able to entrain large amounts of molecular gas, as the molecular outflows they have produced have masses of 4 to 7 M |which is approximately 5 to 10% of the total quiescent gas mass in their parent clouds. These outflows have injected substantial amounts of −1 momentum and kinetic energy on their parent cloud, in the order of 10 M km s and 1044 erg, respectively. We find that both molecular outflows have energies comparable to their parent clouds' turbulent and gravitationally binding energies. In addition, these outflows have been able to redistribute large amounts of their surrounding medium-density (n ∼ 103 cm−3) gas, thereby sculpting their parent cloud and affecting its density and velocity distribution at distances as large as 1 to 1.5 pc from the outflow source. -
Physical Processes in the Interstellar Medium
Physical Processes in the Interstellar Medium Ralf S. Klessen and Simon C. O. Glover Abstract Interstellar space is filled with a dilute mixture of charged particles, atoms, molecules and dust grains, called the interstellar medium (ISM). Understand- ing its physical properties and dynamical behavior is of pivotal importance to many areas of astronomy and astrophysics. Galaxy formation and evolu- tion, the formation of stars, cosmic nucleosynthesis, the origin of large com- plex, prebiotic molecules and the abundance, structure and growth of dust grains which constitute the fundamental building blocks of planets, all these processes are intimately coupled to the physics of the interstellar medium. However, despite its importance, its structure and evolution is still not fully understood. Observations reveal that the interstellar medium is highly tur- bulent, consists of different chemical phases, and is characterized by complex structure on all resolvable spatial and temporal scales. Our current numerical and theoretical models describe it as a strongly coupled system that is far from equilibrium and where the different components are intricately linked to- gether by complex feedback loops. Describing the interstellar medium is truly a multi-scale and multi-physics problem. In these lecture notes we introduce the microphysics necessary to better understand the interstellar medium. We review the relations between large-scale and small-scale dynamics, we con- sider turbulence as one of the key drivers of galactic evolution, and we review the physical processes that lead to the formation of dense molecular clouds and that govern stellar birth in their interior. Universität Heidelberg, Zentrum für Astronomie, Institut für Theoretische Astrophysik, Albert-Ueberle-Straße 2, 69120 Heidelberg, Germany e-mail: [email protected], [email protected] 1 Contents Physical Processes in the Interstellar Medium ............... -
The Veiling Spectrum of DI Cephei and Its Relationship to Emission Line Profiles
A&A 445, 323–329 (2006) Astronomy DOI: 10.1051/0004-6361:20041812 & c ESO 2005 Astrophysics The veiling spectrum of DI Cephei and its relationship to emission line profiles J. F. Gameiro1,2,D.F.M.Folha1,3, and P. P. Petrov 4, 1 Centro de Astrofísica da Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal e-mail: [email protected] 2 Departamento de Matemática Aplicada, Faculdade de Ciências da Universidade do Porto, Portugal 3 Instituto Superior da Maia, Av. Carlos de Oliveira Campos, 4475-690 Avioso S. Pedro, Castelo da Maia, Portugal 4 Crimean Astrophysical Observatory, p/o Nauchny, Crimea, 98409, Ukraine Received 6 August 2004 / Accepted 2 September 2005 ABSTRACT High spectral resolution variability studies of classical T Tauri stars (CTTS) are an essential instrument for probing the physical conditions and dynamics of their atmospheres and immediate vicinity. The shapes of the excess continuum emission and of the line profiles, their variability and relationship are all crucial tools to achieve that goal. We use high spectral resolution optical data of the CTTS DI Cep to suggest a new diagnostic tool to investigate the relationship between the line emission/absorption and the excess continuum emission. By correlating the veiling continuum to the line flux in discrete velocity bins across the emission line we obtain a correlation profile, from which one can discriminate between parts of the line that relate differently to the veiling. An earlier report of an unexpected hump around 5300 Å in the continuum excess emission spectrum of a couple of CTTS is not explained by current models of those stars. -
Research and Scientific Support Department 2003 – 2004
COVER 7/11/05 4:55 PM Page 1 SP-1288 SP-1288 Research and Scientific Research Report on the activities of the Support Department Research and Scientific Support Department 2003 – 2004 Contact: ESA Publications Division c/o ESTEC, PO Box 299, 2200 AG Noordwijk, The Netherlands Tel. (31) 71 565 3400 - Fax (31) 71 565 5433 Sec1.qxd 7/11/05 5:09 PM Page 1 SP-1288 June 2005 Report on the activities of the Research and Scientific Support Department 2003 – 2004 Scientific Editor A. Gimenez Sec1.qxd 7/11/05 5:09 PM Page 2 2 ESA SP-1288 Report on the Activities of the Research and Scientific Support Department from 2003 to 2004 ISBN 92-9092-963-4 ISSN 0379-6566 Scientific Editor A. Gimenez Editor A. Wilson Published and distributed by ESA Publications Division Copyright © 2005 European Space Agency Price €30 Sec1.qxd 7/11/05 5:09 PM Page 3 3 CONTENTS 1. Introduction 5 4. Other Activities 95 1.1 Report Overview 5 4.1 Symposia and Workshops organised 95 by RSSD 1.2 The Role, Structure and Staffing of RSSD 5 and SCI-A 4.2 ESA Technology Programmes 101 1.3 Department Outlook 8 4.3 Coordination and Other Supporting 102 Activities 2. Research Activities 11 Annex 1: Manpower Deployment 107 2.1 Introduction 13 2.2 High-Energy Astrophysics 14 Annex 2: Publications 113 (separated into refereed and 2.3 Optical/UV Astrophysics 19 non-refereed literature) 2.4 Infrared/Sub-millimetre Astrophysics 22 2.5 Solar Physics 26 Annex 3: Seminars and Colloquia 149 2.6 Heliospheric Physics/Space Plasma Studies 31 2.7 Comparative Planetology and Astrobiology 35 Annex 4: Acronyms 153 2.8 Minor Bodies 39 2.9 Fundamental Physics 43 2.10 Research Activities in SCI-A 45 3. -
Infrared Imaging with COAST
Infrared Imaging with COAST John Stephen Young St John’s College, Cambridge and Cavendish Astrophysics A dissertation submitted for the degree of Doctor of Philosophy in the University of Cambridge 26 March 1999 iii Preface This dissertation describes work carried out in the Astrophysics Group of the Department of Phys- ics, University of Cambridge, between October 1995 and March 1999. Except where explicit reference is made to the work of others, this dissertation is the result of my own work, and includes nothing which is the outcome of work done in collaboration. No part of this dissertation has been submitted for a degree, diploma, or other qualification at any University. This dissertation does not exceed 60,000 words in length. v Acknowledgements Many people say that this is the only page of a PhD. thesis worth reading. I hope that is not the case here. This is, however, the only page not written in the passive voice, and the only one which might make you smile. Above all, I would like to thank my supervisor, Professor John Baldwin, for always being available to give advice and encouragement, and for assisting with many hours of alignment and even more hours of observing. The shortbread was much appreciated! Many thanks are also due for his reading of this thesis. It has been a pleasure to work with all of the members of the COAST team. None of the work described in this thesis would have been possible without the NICMOS camera built by Martin Beckett. I would like to thank him for taking the time to explain it to me. -
The Distance to M100 As Determined by Cepheid Variable Stars
Table of Contents The ESA/ESO Astronomy Exercise Series 2 Preface • Preface ..................................................................... page 2 Introduction • Cosmology and distance measurements ......................... page 3 • Using Cepheids as distance estimators .......................... page 5 • M100 a Grand Spiral ................................................... page 7 Tasks • Measurements and calculations .................................... page 8 • Task 1 ...................................................................... page 8 • Task 2 ...................................................................... page 9 • Task 3 ...................................................................... page 10 • Task 4 ...................................................................... page 10 • Task 5 ...................................................................... page 10 • Task 6 ...................................................................... page 11 • Task 7 ...................................................................... page 11 • Task 8 ...................................................................... page 11 Table of Contents of Table Further Reading • Scientific papers ........................................................ page 12 Teacher’s Guide • Teacher’s Guide .......................................................... page 14 1 Preface The ESA/ESO Astronomy Exercise Series 2 The Distance to M100 as Determined by Cepheid Variable Stars Astronomy is an accessible and visual science, -
Oregon Star Party Advanced Observing List
Welcome to the OSP Advanced Observing List In a sincere attempt to lure more of you into trying the Advanced List, each object has a page telling you what it is, why it’s interesting to observe, and the minimum size telescope you might need to see it. I’ve included coordinates, the constellation each object is located in, and either a chart or photo (or both) showing what the object looks like and how it’s situated in the sky. All you have to do is observe and enjoy the challenge. Stretch your skill and imagination - see something new, something unimaginably old, something unexpected Even though this is a challenging list, you don’t need 20 years of observing experience or a 20 inch telescope to be successful – although in some cases that will help. The only way to see these cool objects for yourself is to give them a go. Howard Banich, The minimum aperture listed for each object is a rough estimate. The idea is to Chuck Dethloff and show approximately what size telescope might be needed to successfully observe Matt Vartanian that particular object. The range is 3 to 28 inches. collaborated on this The visibility of each object assumes decently good OSP observing conditions. year’s list. Requirements to receive a certificate 1. There are 14 objects to choose from. Descriptive notes and/or sketches that clearly show you observed 10 objects are needed to receive the observing certificate. For instance, you can mark up these photos and charts with lines and arrows, and add a few notes describing what you saw.