Radial Velocity Detection of Extra-Solar Planetary Systems
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The Discovery of HD 37605C and a Dispositive Null Detection Of
A Preprint typeset using LTEX style emulateapj v. 5/2/11 THE DISCOVERY OF HD 37605c AND A DISPOSITIVE NULL DETECTION OF TRANSITS OF HD 37605b1 Sharon Xuesong Wang (王雪凇)2,3,Jason T. Wright2,3, William Cochran4, Stephen R. Kane5, Gregory W. Henry6, Matthew J. Payne7, Michael Endl4, Phillip J. MacQueen4, Jeff A. Valenti8, Victoria Antoci9,10, Diana Dragomir9, Jaymie M. Matthews9, Andrew W. Howard11,12, Geoffrey W. Marcy11, Howard Isaacson11, Eric B. Ford7, Suvrath Mahadevan2,3, and Kaspar von Braun5 ABSTRACT We report the radial-velocity discovery of a second planetary mass companion to the K0 V star HD 37605, which was already known to host an eccentric, P 55 days Jovian planet, HD 37605b. This second planet, HD 37605c, has a period of 7.5 years with∼ a low eccentricity and an M sin i of ∼ 3.4 MJup. Our discovery was made with the nearly 8 years of radial velocity follow-up at the Hobby- Eberly∼ Telescope and Keck Observatory, including observations made as part of the Transit Ephemeris Refinement and Monitoring Survey (TERMS) effort to provide precise ephemerides to long-period planets for transit follow-up. With a total of 137 radial velocity observations covering almost eight years, we provide a good orbital solution of the HD 37605 system, and a precise transit ephemeris for HD 37605b. Our dynamic analysis reveals very minimal planet-planet interaction and an insignificant transit time variation. Using the predicted ephemeris, we performed a transit search for HD 37605b with the photometric data taken by the T12 0.8-m Automatic Photoelectric Telescope (APT) and the Microvariability and Oscillations of Stars (MOST) satellite. -
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 -
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 ............... -
Can There Be an Earth-Like Planet in HD 37605?
Can there be an Earth-like planet in HD 37605? Johan Appelgren Lund Observatory Lund University 2017-EXA124 Degree project of 15 higher education credits May 2017 Supervisor: Melvyn Davies Lund Observatory Box 43 SE-221 00 Lund Sweden Abstract Detection of Earth-mass planets on orbits around 1 AU with the radial velocity method has so far not been possible, the Doppler velocity they induce on their host star is too small to be detected. Planetary systems detected with the radial velocity method might then contain undetected Earth-like planets. One such planetary system is HD37605, which contains a star similar to the Sun and two gas giants. One on a highly eccentric low semi- major axis orbit, and one on a near circular orbit almost 4 AU out. In this thesis the possibility that an Earth-like planet, with 1 M⊕ or 2 M⊕ masses, can remain on stable orbits within the habitable zone of HD37605 is investigated. This is done by simulating HD37605 with an additional planet for 20 Myr using the Mercury package. Orbits are considered stable if the simulations does not end in an ejection or collision, and they are considered habitable if the additional planet never leaves the habitable zone. It was found that stability varies a lot over the habitable zone. Peak stability occurs at 0.9 AU and 1.2 AU, and peak instability at 1.1 AU. Habitable runs were found in a region between 0.95 AU and 1 AU. This was the only region where the eccentricity oscillations induced on the additional planet can remain small enough that the planet does not leave the habitable zone. -
Radial Velocity Detection of Extra-Solar Planetary Systems” 1 June 2003 to 31 May 2004 Mcdonald Observatory, the University of Texas Principal Investigator: Dr
Summary of Research for NASA Grant NAG5-13206 “Radial Velocity Detection of Extra-Solar Planetary Systems” 1 June 2003 to 31 May 2004 McDonald Observatory, The University of Texas Principal Investigator: Dr. William D. Cochran This NASA Origins Program grant supported four closely related research programs at The University of Texas at Austin: 1) The McDonald Observatory Planetary Search (MOPS) Program, using the McDonald Observatory 2.7m Harlan Smith telescope and its 2dcoudd spectrometer, 2) A high-precision radial-velocity survey of Hyades dwarfs, using the Keck telescope and its HIRES spectrograph, 3) A program at McDonald Observatory to obtain spectra of the parent stars of planetary systems at R = 210,000, and 4) the start of high precision radial velocity surveys using the Hobby-Eberly Telescope. The most important results from NASA support of these research programs are described below. A list of all papers published under support of this grant is included at the end. The 2.7m McDonald Observatory Planetary Search (MOPS) During this grant, we started de-emphasizing the 2.7m program, as this instrument is capable of achieving only about 6-8ms-’ radial velocity precision, and the observations are quite labor intensive. We are now requesting 6 observing runs per year with the 2.7m 2dcoudd spectrograph of 3-4 nights each. We are targeting this program to the specific niches where it can still make a significant contribution. The 2.7m MOPS target list now includes about 270 stars. A brown-dwarf companion to HD 137510. Since the beginning of precise Doppler surveys, one surprising enigma has emerged: the relative paucity of spectroscopic binaries where the secondary mass lies in between the stellar and planetary mass regime. -
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. -
Ricky Leon Murphy Project
Ricky Leon Murphy The Appendices: Project – HET606 Appendix 1 – Known Exoplanets Semester 2 – 2004 Appendix 2 – Location of Tau Bootis Appendix 3 – Location of HD 209458 Appendix 4 – Image Reduction Search for Other Worlds Introduction As of September 2004, there are 136 known planets outside our solar system (http://exoplanets.org). These extra-solar planets, or exoplanets, are one of the most current and highly studied subjects in Astronomy today and it is one of the very few subjects that involve both amateur and professional astronomers. The huge telescopes perched atop Mauna Kea in Hawaii are pointed at these objects, as are 8” telescopes purchased from the local shopping mall – and many others around the world. Why are we finding these planets now if only 8” telescopes can detect them? Simple; we know what we are looking for and we have better tools to get the job done. While telescope size does not seem to matter with the search and study of exoplanets, it’s what you do not hear about that really matters: improved sensitivity in CCD cameras, improved resolution in spectroscopy, and fast computers to perform the mathematics. The goal of gathering repeatable data is very important when studying exoplanets. The rewards of such study carry implications across the board in Astronomy: we can learn about our own solar system and test the theories of solar system formation and evolution, improve the sensitivity to detect small Earth-like planets, and possibly provide targets for the spaced based telescopes and SETI projects; however, the most important implication is that perhaps for the first time in history, amateurs and professionals from around the world are engaged in this subject and working together to share the data. -
OCTOBER 2009 OBSERVER Inside the the Chill’S A-Comin’ Observer
THE DENVER OBSERVER OCTOBER 2009 OBSERVER Inside the The Chill’s a-Comin’ Observer President’s Corner........................... 2 Society Directory............................. 2 Prelude Lake................................... 3 New Scope Operator......................... 5 New Members.................................. 5 Astronomical League....................... 6 NASA’S Space Place......................... 7 Schedule of Events.............. back page Calendar 4.................................................... Full moon BUT NOWHERE NEAR THE TEMPERATURE INSIDE THE MU CEPHEI NEBULA 11..................................... Last quarter moon CLOUD, IC 1396 IN CEPHEUS, WHERE A FRIGID -290ᵒ AWAITS A STELLAR ADVENTURER 17.................................................. New moon Joe used an SBIG ST-2000XM ccd camera with a 110mm Mamiya RZ lens at f/5.6. Please contact Joe for more technical details. The bright orange star is Mu Cephei, the Garnet Star; 24........................ Colorado Astronomy Day the Elephant Trunk nebula portion is right of center. 25.................................... First quarter moon Image copyright 2009 Joe Gafford OCTOBER SKIES by Dennis Cochran upiter is already up in the south when darkness descends, situated along Alpha Aquarius, the star at the top of the arc of that constellation. Above it J the top left of Capricornus’ goat-ee jester grin. Above Jupiter and the a short way and a bit west is the slightly brighter red star, Enif, at the end of Goat is the water jug of Aquarius, in case you’ve ever wondered where one of Pegasus’ legs. Just northwest of Enif is M15, one of the best globulars this elusive constellation lies. Wasn’t there an Age of Aquarius? Perhaps that on the list. If you then drop from Enif or M15, straight south about 2/3 of was when the New Age movement was born. -
Determining the True Mass of Radial-Velocity Exoplanets with Gaia 9 Planet Candidates in the Brown-Dwarf/Stellar Regime and 27 Confirmed Planets
Astronomy & Astrophysics manuscript no. exoplanet_mass_gaia c ESO 2020 September 30, 2020 Determining the true mass of radial-velocity exoplanets with Gaia 9 planet candidates in the brown-dwarf/stellar regime and 27 confirmed planets F. Kiefer1; 2, G. Hébrard1; 3, A. Lecavelier des Etangs1, E. Martioli1; 4, S. Dalal1, and A. Vidal-Madjar1 1 Institut d’Astrophysique de Paris, Sorbonne Université, CNRS, UMR 7095, 98 bis bd Arago, 75014 Paris, France 2 LESIA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, Université de Paris, 5 place Jules Janssen, 92195 Meudon, France? 3 Observatoire de Haute-Provence, CNRS, Universiteé d’Aix-Marseille, 04870 Saint-Michel-l’Observatoire, France 4 Laboratório Nacional de Astrofísica, Rua Estados Unidos 154, 37504-364, Itajubá - MG, Brazil Submitted on 2020/08/20 ; Accepted for publication on 2020/09/24 ABSTRACT Mass is one of the most important parameters for determining the true nature of an astronomical object. Yet, many published exoplan- ets lack a measurement of their true mass, in particular those detected thanks to radial velocity (RV) variations of their host star. For those, only the minimum mass, or m sin i, is known, owing to the insensitivity of RVs to the inclination of the detected orbit compared to the plane-of-the-sky. The mass that is given in database is generally that of an assumed edge-on system (∼90◦), but many other inclinations are possible, even extreme values closer to 0◦ (face-on). In such case, the mass of the published object could be strongly underestimated by up to two orders of magnitude. -
Evidence for Enhanced Chromospheric Ca II H and K Emission in Stars with Close-In Extrasolar Planets
A&A 540, A82 (2012) Astronomy DOI: 10.1051/0004-6361/201118247 & c ESO 2012 Astrophysics Evidence for enhanced chromospheric Ca II H and K emission in stars with close-in extrasolar planets T. Krejcovᡠ1 and J. Budaj2 1 Department of Theoretical Physics and Astrophysics, Masaryk University, Kotlárskᡠ2, 61137 Brno, Czech Republic e-mail: [email protected] 2 Astronomical Institute, Slovak Academy of Sciences, 05960 Tatranská Lomnica, Slovak Republic e-mail: [email protected] Received 11 October 2011 / Accepted 13 February 2012 ABSTRACT Context. The planet-star interaction is manifested in many ways. It has been found that a close-in exoplanet causes small but mea- surable variability in the cores of a few lines in the spectra of several stars, which corresponds to the orbital period of the exoplanet. Stars with and without exoplanets may have different properties. Aims. The main goal of our study is to search for the influence that exoplanets might have on atmospheres of their host stars. Unlike the previous studies, we do not study changes in the spectrum of a host star or differences between stars with and without exoplanets. We aim to study a large number of stars with exoplanets and the current level of their chromospheric activity and to look for a possible correlation with the exoplanetary properties. Methods. To analyse the chromospheric activity of stars, we exploited our own and publicly available archival spectra, measured the equivalent widths of the cores of Ca II H and K lines, and used them to trace their activity. Subsequently, we searched for their dependence on the orbital parameters and the mass of the exoplanet. -
Chromospheric Activity Induced by Short-Period Planets a Search for Modulation of Ca II H &; K Emission
Chromospheric Activity Induced by Short-Period Planets A Search for Modulation of Ca II H &; K Emission by Evgenya Shkolnik B.Sc. (Physics and Mathematics), Dalhousie University, 1998 M.Sc. (Astronomy), The University of British Columbia, 2000 A THESIS SUBMITTED IN PARTIAL FULFILMENT OF THE REQUIREMENTS FOR THE DEGREE OF DOCTOR OF PHILOSOPHY in The Faculty of Graduate Studies (Department of Physics and Astronomy) We accept this thesis as conforming to the required standard THE UNIVERSITY OF BRITISH COLUMBIA December 4, 2003 © Evgenya Shkolnik, 2003 Abstract I have detected the first evidence of magnetic interaction between an extra- solar planet and its parent star. Of the > 100 extrasolar planets discovered to date, approximated 20% of them are '51 Peg'-type with a Jupiter-mass planet orbiting within 0.1 As- tronomical Units. The systems with the tightest orbits (P orb < 5 days) offer the best opportunity to observe a tidal or magnetic interaction between the planet and its parent star. Stellar chromospheric activity could be modu- lated in two ways. For magnetic interaction, the modulation is predicted to be at the orbital period with enhancement near the sub-planetary point (</> = 0). Tidal interaction would stimulate activity with a period of Porb/2 with enhancements near both <j> — 0 and 0.5. The Ca II H & K line reversals at 3968 and 3933 A are the best chro- mospheric activity indicators visible from the ground. I observed the H & K emission cores of five sun-like stars with short period planets: r Boo, HD179949, HD 209458, 51 Peg and v And. -
Jupiter Analogs Orbit Stars with an Average Metallicity Close to That of the Sun
Downloaded from orbit.dtu.dk on: Oct 05, 2021 Jupiter Analogs Orbit Stars with an Average Metallicity Close to That of the Sun Buchhave, Lars A.; Bitsch, Bertram; Johansen, Anders; Latham, David W.; Bizzarro, Martin; Bieryla, Allyson; Kipping, David M. Published in: Astrophysical Journal Link to article, DOI: 10.3847/1538-4357/aaafca Publication date: 2018 Document Version Publisher's PDF, also known as Version of record Link back to DTU Orbit Citation (APA): Buchhave, L. A., Bitsch, B., Johansen, A., Latham, D. W., Bizzarro, M., Bieryla, A., & Kipping, D. M. (2018). Jupiter Analogs Orbit Stars with an Average Metallicity Close to That of the Sun. Astrophysical Journal, 856(1), [37]. https://doi.org/10.3847/1538-4357/aaafca General rights Copyright and moral rights for the publications made accessible in the public portal are retained by the authors and/or other copyright owners and it is a condition of accessing publications that users recognise and abide by the legal requirements associated with these rights. Users may download and print one copy of any publication from the public portal for the purpose of private study or research. You may not further distribute the material or use it for any profit-making activity or commercial gain You may freely distribute the URL identifying the publication in the public portal If you believe that this document breaches copyright please contact us providing details, and we will remove access to the work immediately and investigate your claim. The Astrophysical Journal, 856:37 (11pp), 2018 March 20 https://doi.org/10.3847/1538-4357/aaafca © 2018.