DOCSLIB.ORG

An Ultra-Hot Jupiter Transiting HR5599 in a Polar Orbit

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
An Ultra-Hot Jupiter Transiting HR5599 in a Polar Orbit MNRAS 000, 1–10 (2018) Preprint 14 September 2018 Compiled using MNRAS LATEX style file v3.0 WASP-189b: an ultra-hot Jupiter transiting the bright A star HR5599 in a polar orbit⋆ D. R. Anderson,1 L. Y. Temple,1 L. D. Nielsen,2 A. Burdanov,3 C. Hellier,1 † F. Bouchy,2 D. J. A. Brown,4,5 A. Collier Cameron,6 M. Gillon,3 E. Jehin,3 P. F. L. Maxted,1 F. Pepe,2 D. Pollacco,4,5 F. J. Pozuelos,3 D. Queloz,2,7 D. S´egransan,2 B. Smalley,1 A. H. M. J. Triaud,8 O. D. Turner,2 S. Udry2 and R. G. West4,5 1Astrophysics Group, Keele University, Staffordshire ST5 5BG, UK 2Observatoire de Gen`eve, Universit´ede Gen`eve, 51 Chemin des Maillettes, 1290 Sauverny, Switzerland 3Space sciences, Technologies and Astrophysics Research (STAR) Institute, Universit´ede Li`ege, Li`ege 1, Belgium 4Department of Physics, University of Warwick, Coventry CV4 7AL, UK 5Centre for Exoplanets and Habitability, University of Warwick, Gibbet Hill Road, Coventry CV4 7AL, UK 6SUPA, School of Physics and Astronomy, University of St. Andrews, North Haugh, Fife KY16 9SS, UK 7Cavendish Laboratory, J J Thomson Avenue, Cambridge CB3 0HE, UK 8School of Physics & Astronomy, University of Birmingham, Edgbaston, Birmingham, B15 2TT, UK Accepted XXX. Received YYY; in original form 2018 September 13 ABSTRACT We report the discovery of WASP-189b: an ultra-hot Jupiter in a 2.72-d transiting orbit around the V = 6.6 A star WASP-189 (HR 5599). We detected periodic dim- mings in the star’s lightcurve, first with the WASP-South survey facility then with the TRAPPIST-South telescope. We confirmed that a planet is the cause of those dim- mings via line-profile tomography and radial-velocity measurements using the HARPS and CORALIE spectrographs. Those reveal WASP-189b to be an ultra-hot Jupiter (MP = 2.13 0.28 MJup; RP = 1.374 0.082 RJup) in a polar orbit (λ = 89.3 1.4 ; ± ± ± ◦ Ψ = 90.0 5.8◦) around a rapidly rotating A6IV–V star (Teff = 8000 100 K; v sin i ±1 ± ∗ ∗ ≈ 100km s− ). We calculate a predicted equilibrium temperature of Teql = 2641 34 K, assuming zero albedo and efficient redistribution, which is the third hottest± for the known exoplanets. WASP-189 is the brightest known host of a transiting hot Jupiter and the third-brightest known host of any transiting exoplanet. We note that of the eight hot-Jupiter systems with Teff > 7000 K, seven have strongly misaligned orbits, and two of the three systems with Teff 8000 K have polar orbits (the third is aligned). ≥ Key words: planets and satellites: detection – planets and satellites: individual: arXiv:1809.04897v1 [astro-ph.EP] 13 Sep 2018 WASP-189b – stars: individual: WASP-189 – stars: individual: HR 5599 1 INTRODUCTION tive temperature Teff > 7000 K. This is because the spectral lines of very hot, rapidly rotating stars are sparse and broad, With 750 transiting planets well studied the emphasis is ∼ which complicates the radial-velocity verification of planets. on pushing planet discovery into regimes where there are Hence we know little about the formation and evolution of few known planets. Of the 580 host stars listed in the TEP- planets around hot stars. Cat database (Southworth 2011), only 9 have stellar effec- Under the core accretion model of planet formation, giant planets are expected to be more common around ⋆ Based on observations collected at the European Organisation more massive stars (Pollack et al. 1996), with an occurrence for Astronomical Research in the Southern Hemisphere under rate predicted by Kennedy & Kenyon (2008) to increase lin- ESO programme 0100.C-0847. early with stellar mass over the range 0.4–3 M . Indeed, ⊙ E-mail: [email protected] Cumming et al. (2008) found that the occurrence rate of gi- † © 2018 The Authors 2 D. R. Anderson et al. M M P ant planets (planet mass P = 0.3–10 Jup; orbital period 1.01 = 2–2000 d) is ten times lower for M dwarfs (1 per cent) than for FGK stars (10.5 per cent). Whether this trend contin- ues to A stars is unknown. Borgniet et al. (2017) reported +10 M an occurrence rate of 4 4 per cent for A-type stars ( P = 1 0.1–10 MJup; P = 1–1000− d), which is too imprecise to tell. An additional motivation to discover planets around hot Relative flux stars is their potential for characterisation. As hot stars are intrinsically luminous, many bright stars (which are eas- 0.99 ier to study) are hot stars: of the Bright Star Catalogue 0.4 0.6 0.8 1 1.2 1.4 1.6 (Hoffleit & Jaschek 1991), 41 per cent are listed as OBA Orbital phase stars and 21 per cent are listed as A stars. Also, plan- ets in close orbits around hot stars are intensely irradi- Figure 1. ated, which facilitates the probing of their atmospheres. For WASP-South survey lightcurve folded on the adopted ephemeris from Table 3 and binned (bin width equivalent to example, a great deal of work has been done to charac- 2 min). terise the atmosphere of WASP-33b (Collier Cameron et al. 2010b; Teff = 7430 K; V = 8.2; P = 1.22 d) from detections of its thermal emission (Smith et al. 2011; Deming et al. 2012; Using HARPS on the ESO 3.6-m telescope (Pepe et al. de Mooij et al. 2013; Haynes et al. 2015; von Essen et al. 2000), we obtained a series of spectra during the tran- 2015; Nugroho et al. 2017; Zhang et al. 2018). sit night of 2018 Mar 26. Using the HARPS Data Re- In their initial configuration the WASP survey facil- duction Software (DRS), we computed average stellar line ities operated with 200-mm f/1.8 lenses, as described by profiles, or cross-correlation functions (CCFs), by cross- Pollacco et al. (2006), targetting stars in the range V = 9– correlating the HARPS spectra with a weighted A0 binary 13. WASP-South ran in this mode from 2006 to 2012, re- mask from which we had removed various tellurics and ISM sulting in the discovery of 125 planets (some jointly with lines (Baranne et al. 1996; Pepe et al. 2002). The time-series SuperWASP-North). But WASP-South saturated at V = 9, of these CCFs constitute the HARPS Doppler tomography and the brightest planet-host found in the South was WASP- data set, DTHAR. We discarded the last two spectra of the se- 18 at V = 9.3 (Hellier et al. 2009). Since several brighter ries as they were visibly affected by twilight. In the resulting hosts were known in the North we decided to switch to tomogram (top-left panel of Fig. 2), there is a trace indica- Canon 85-mm f/1.2 lenses, with an SDSS r-band filter and tive of a planet in a polar orbit crossing the red-shifted hemi- shorter exposures (three 20-s exposures per pointing instead sphere of the star. However, due to ephemeris uncertainty of two 30-s exposures), so covering the range V = 6.5–11. (our initial attempts to refine the ephemeris with additional WASP-South ran in this configuration from 2012 to 2015. transit photometry were unsuccessful) we had missed the This survey mode is similar to that of the KELT ingress of the event and we were concerned about possible project (Pepper et al. 2007), which uses a Mamiya 80- lunar contamination. The Moon, which was 77 per cent illu- mm f/1.9 lens, and which has been vindicated by spec- minated and at a distance of 95 from the target, had set ∼ ◦ tacular discoveries such as KELT-9 (Gaudi et al. 2017) at 06:46 UT. The barycentric Earth velocity was 18.5 km 1 and KELT-20/MASCARA-2 (Lund et al. 2017; Talens et al. s− . The trace in the tomogram occurs at a similar veloc- 2018), which are both V = 7.6 systems. KELT-9b, which ity and is apparent in the CCFs taken up to 06:04 UT. We transits the hottest known hot-Jupiter host (T 10 200 K), eff≈ cross-correlated with the A0 mask the sky spectra taken si- is already proving invaluable for atmospheric characterisa- multaneously using the secondary HARPS fibre and found tion (Hoeijmakers et al. 2018). no signal (Fig. 3), which indicates that the signal in the In this paper we present the discovery of WASP-189b, target tomogram is not due to the Moon. an ultra-hot Jupiter transiting an even brighter star, being Using CORALIE, we obtained a series of spectra dur- in a polar orbit around the mid-A star WASP-189 (HR 5599; ing the transit night of 2018 Jul 13. The Moon posed no V = T 6.6; eff = 8000 K). issue as it was only 2 per cent illuminated and it set at 23:01 UT (26 min before the CORALIE sequence began). We again computed CCFs using the A0 mask to produce 2 PHOTOMETRIC AND SPECTROSCOPIC the CORALIE Doppler tomography data set, DTCOR. In OBSERVATIONS the resulting tomogram (top-right panel of Fig. 2), there is a trace indicative of a planet in a polar orbit crossing the We present in Table 1 a summary of our photometric red-shifted hemisphere of the star. This is similar to the and spectroscopic observations of WASP-189. We observed trace in the DTHARPS tomogram, which occurs at a similar WASP-189 during 2012 Jul to 2013 Aug with the modified barcyentric RV.
Load more

Recommended publications
  • Astrodynamics
    Politecnico di Torino SEEDS SpacE Exploration and Development Systems Astrodynamics II Edition 2006 - 07 - Ver. 2.0.1 Author: Guido Colasurdo Dipartimento di Energetica Teacher: Giulio Avanzini Dipartimento di Ingegneria Aeronautica e Spaziale e-mail: [email protected] Contents 1 Two–Body Orbital Mechanics 1 1.1 BirthofAstrodynamics: Kepler’sLaws. ......... 1 1.2 Newton’sLawsofMotion ............................ ... 2 1.3 Newton’s Law of Universal Gravitation . ......... 3 1.4 The n–BodyProblem ................................. 4 1.5 Equation of Motion in the Two-Body Problem . ....... 5 1.6 PotentialEnergy ................................. ... 6 1.7 ConstantsoftheMotion . .. .. .. .. .. .. .. .. .... 7 1.8 TrajectoryEquation .............................. .... 8 1.9 ConicSections ................................... 8 1.10 Relating Energy and Semi-major Axis . ........ 9 2 Two-Dimensional Analysis of Motion 11 2.1 ReferenceFrames................................. 11 2.2 Velocity and acceleration components . ......... 12 2.3 First-Order Scalar Equations of Motion . ......... 12 2.4 PerifocalReferenceFrame . ...... 13 2.5 FlightPathAngle ................................. 14 2.6 EllipticalOrbits................................ ..... 15 2.6.1 Geometry of an Elliptical Orbit . ..... 15 2.6.2 Period of an Elliptical Orbit . ..... 16 2.7 Time–of–Flight on the Elliptical Orbit . .......... 16 2.8 Extensiontohyperbolaandparabola. ........ 18 2.9 Circular and Escape Velocity, Hyperbolic Excess Speed . .............. 18 2.10 CosmicVelocities
    [Show full text]
  • Arxiv:1505.07033V2 [Astro-Ph.IM] 4 Sep 2015
    September 7, 2015 0:46 manuscript Journal of Astronomical Instrumentation c World Scientific Publishing Company A CUBESAT FOR CALIBRATING GROUND-BASED AND SUB-ORBITAL MILLIMETER-WAVE POLARIMETERS (CALSAT) Bradley R. Johnson1, Clement J. Vourch2, Timothy D. Drysdale2, Andrew Kalman3, Steve Fujikawa4, Brian Keating5 and Jon Kaufman5 1Department of Physics, Columbia University, New York, NY 10027, USA 2School of Engineering, University of Glasgow, Glasgow, Scotland G12 8QQ, UK 3Pumpkin, Inc., San Francisco, CA 94112, USA 4Maryland Aerospace Inc., Crofton, MD 21114, USA 5Department of Physics, University of California, San Diego, CA 92093-0424, USA Received (to be inserted by publisher); Revised (to be inserted by publisher); Accepted (to be inserted by publisher); We describe a low-cost, open-access, CubeSat-based calibration instrument that is designed to support ground- based and sub-orbital experiments searching for various polarization signals in the cosmic microwave background (CMB). All modern CMB polarization experiments require a robust calibration program that will allow the effects of instrument-induced signals to be mitigated during data analysis. A bright, compact, and linearly polarized astrophysical source with polarization properties known to adequate precision does not exist. Therefore, we designed a space-based millimeter-wave calibration instrument, called CalSat, to serve as an open-access calibrator, and this paper describes the results of our design study. The calibration source on board CalSat is composed of five \tones" with one each at 47.1, 80.0, 140, 249 and 309 GHz. The five tones we chose are well matched to (i) the observation windows in the atmospheric transmittance spectra, (ii) the spectral bands commonly used in polarimeters by the CMB community, and (iii) The Amateur Satellite Service bands in the Table of Frequency Allocations used by the Federal Communications Commission.
    [Show full text]
  • Up, Up, and Away by James J
    www.astrosociety.org/uitc No. 34 - Spring 1996 © 1996, Astronomical Society of the Pacific, 390 Ashton Avenue, San Francisco, CA 94112. Up, Up, and Away by James J. Secosky, Bloomfield Central School and George Musser, Astronomical Society of the Pacific Want to take a tour of space? Then just flip around the channels on cable TV. Weather Channel forecasts, CNN newscasts, ESPN sportscasts: They all depend on satellites in Earth orbit. Or call your friends on Mauritius, Madagascar, or Maui: A satellite will relay your voice. Worried about the ozone hole over Antarctica or mass graves in Bosnia? Orbital outposts are keeping watch. The challenge these days is finding something that doesn't involve satellites in one way or other. And satellites are just one perk of the Space Age. Farther afield, robotic space probes have examined all the planets except Pluto, leading to a revolution in the Earth sciences -- from studies of plate tectonics to models of global warming -- now that scientists can compare our world to its planetary siblings. Over 300 people from 26 countries have gone into space, including the 24 astronauts who went on or near the Moon. Who knows how many will go in the next hundred years? In short, space travel has become a part of our lives. But what goes on behind the scenes? It turns out that satellites and spaceships depend on some of the most basic concepts of physics. So space travel isn't just fun to think about; it is a firm grounding in many of the principles that govern our world and our universe.
    [Show full text]
  • Standard Candles in Cosmology
    Standard Candles: Distance Measurement in Astronomy Farley V. Ferrante Southern Methodist University 5/3/2017 PHYS 3368: Principles of Astrophysics & Cosmology 1 OUTLINE • Cosmic Distance Ladder • Standard Candles Parallax Cepheid variables Planetary nebula Most luminous supergiants Most luminous globular clusters Most luminous H II regions Supernovae Hubble constant & red shift • Standard Model of Cosmology 5/3/2017 PHYS 3368: Principles of Astrophysics & Cosmology 2 The Cosmic Distance Ladder - Distances far too vast to be measured directly - Several methods of indirect measurement - Clever methods relying on careful observation and basic mathematics - Cosmic distance ladder: A progression of indirect methods which scale, overlap, & calibrate parameters for large distances in terms of smaller distances • More methods calibrate these distances until distances that can be measured directly are achieved 5/3/2017 PHYS 3368: Principles of Astrophysics & Cosmology 3 Standard Candles • Magnitude: Historical unit (Hipparchus) of stellar brightness such that 5 magnitudes represents a factor of 100 in intensity • Apparent magnitude: Number assigned to visual brightness of an object; originally a scale of 1-6 • Absolute magnitude: Magnitude an object would have at 10 pc (convenient distance for comparison) • List of most luminous stars 5/3/2017 PHYS 3368: Principles of Astrophysics & Cosmology 4 5/3/2017 PHYS 3368: Principles of Astrophysics & Cosmology 5 The Cosmic Distance Ladder 5/3/2017 PHYS 3368: Principles of Astrophysics & Cosmology 6 The
    [Show full text]
  • GW Librae: a Unique Laboratory for Pulsations in an Accreting White Dwarf
    MNRAS 000,1–11 (2016) Preprint 11 April 2016 Compiled using MNRAS LATEX style file v3.0 GW Librae: A unique laboratory for pulsations in an accreting white dwarf O. Toloza,1? B. T. G¨ansicke,1 J. J. Hermes,2;19 D. M. Townsley,3 M. R. Schreiber4, P. Szkody5, A. Pala1, K. Beuermann6, L. Bildsten7, E. Breedt1, M. Cook8;10, P. Godon9, A. A. Henden10, I. Hubeny11, C. Knigge12, K. S. Long13, T. R. Marsh1, D. de Martino14, A. S. Mukadam5;15, G. Myers10, P. Nelson 16, A. Oksanen9;17, J. Patterson18, E. M. Sion9, M. Zorotovic4 1Department of Physics, University of Warwick, Coventry - CV4 7AL, UK 2Department of Physics and Astronomy, University of North Carolina, Chapel Hill, NC 27599-3255, USA 3Department of Physics and Astronomy, The University of Alabama, Tuscaloosa, AL - 35487, USA 4Instituto de F½sica y Astronom½a, Universidad de Valpara½so, Valpara½so, 2360102, Chile 5Department of Astronomy, University of Washington, Seattle, WA - 98195-1580, USA 6Institut f¨urAstrophysik Friedrich-Hund-Platz 1, Georg-August-Universit¨at,G¨ottingen,37077, Germany 7Kavli Institute for Theoretical Physics and Department of Physics Kohn Hall, University of California, Santa Barbara, CA 93106, USA 8Newcastle Observatory, Newcastle, ON L1B 1M5 Canada 9Astrophysics and Planetary Science, Villanova University, Villanova, PA 19085, USA 10American Association Of Variable Star Observers 11Steward Observatory and Dept. of Astronomy, University of Arizona, Tucson, AZ 85721, USA 12School of Physics and Astronomy, University of Southampton, Southampton, SO17 1BJ, UK 13Space Telescope Science Institute, Baltimore, MD 21218, USA 14Osservatorio Astronomico di Capodimonte, salita Moiariello 16, 80131 Napoli, Italy 15Apache Point Observatory, 2001 Apache Point Road, Sunspot, NM 88349-0059, USA 161105 Hazeldean Rd, Ellinbank 3820, Australia 17Caisey Harlingten Observatory, San Pedro de Atacama, Chile 18Department of Astronomy, Columbia University, New York, NY 10027, USA 19Hubble Fellow Accepted XXX.
    [Show full text]
  • Jupiter Analogues and Planets of Acave Stars
    Jupiter analogues and planets of ac2ve stars. RV searches at MPIA Heidelberg Mar2n Kürster with Maren Mohler-Fischer (1) Jupiter analogues: The planet search programme at the ESO CES and HAPRS. IV. The search for Jupiter analogues around solar-type stars, Zechmeister, Kürster, Endl, Lo Curto, Hartman, Nilsson, Henning, Hatzes, Cochran, 2012, A&A accepted (2) A search for planets around ac2ve stars. Mohler-Fischer, Henning, Launhardt, Müller, Guenther (work in progress) (3) The first RV-confirmed planet from HAT-South: HATS-1b: The first transiGng plamet discovered by the HATSOUTH survey, Penev, Bakos, Bayliss, Jordán, Mohler-Fischer, Zhou, Suc, Rabus, Hartman, Mancini, Béky, Zsurby, Buchhave, Henning, Nikolov, Csák, Brahm, Espinosa, Conroy, Noyes, Sasselov, Schmidt, Wright, Tinney, Addison, Lásár, Papp, Sári 2012, in prep. La Silla Observatory, ESO, Chile Hot Planets and Cool Stars MPE Garching 13 November 2012 M. Kürster ad (2): A search for planets around ac2ve stars. Mohler-Fischer, Henning, Launhardt, Müller, Guenther (work in progress) G9V star, v sin i = 20.8 km/s, 57 spectra taken with FEROS @ MPG/ESO 2.2m La Silla Variaon due to stellar ac2vity / surface features Hot Planets and Cool Stars MPE Garching 13 November 2012 M. Kürster ad (3): HATS-1b See yesterday’s talk by Gaspar Bakos RV confirma2on: CORALIE: filled circles àFEROS: open triangles CYCLOPS: filled triangles Hot Planets and Cool Stars MPE Garching 13 November 2012 M. Kürster Two talks you cannot miss: Nadia Kostogryz ``A spectral differenLal characterizaon of low-mass companions´´ This aernoon, but unfortunately cancelled: Florian Rodler ``The return of the mummy: evidence for starlight reflected from the massive hot Jupiter τ Boo b´´ Hot Planets and Cool Stars MPE Garching 13 November 2012 M.
    [Show full text]
  • Mission Design for the Lunar Reconnaissance Orbiter
    AAS 07-057 Mission Design for the Lunar Reconnaissance Orbiter Mark Beckman Goddard Space Flight Center, Code 595 29th ANNUAL AAS GUIDANCE AND CONTROL CONFERENCE February 4-8, 2006 Sponsored by Breckenridge, Colorado Rocky Mountain Section AAS Publications Office, P.O. Box 28130 - San Diego, California 92198 AAS-07-057 MISSION DESIGN FOR THE LUNAR RECONNAISSANCE ORBITER † Mark Beckman The Lunar Reconnaissance Orbiter (LRO) will be the first mission under NASA’s Vision for Space Exploration. LRO will fly in a low 50 km mean altitude lunar polar orbit. LRO will utilize a direct minimum energy lunar transfer and have a launch window of three days every two weeks. The launch window is defined by lunar orbit beta angle at times of extreme lighting conditions. This paper will define the LRO launch window and the science and engineering constraints that drive it. After lunar orbit insertion, LRO will be placed into a commissioning orbit for up to 60 days. This commissioning orbit will be a low altitude quasi-frozen orbit that minimizes stationkeeping costs during commissioning phase. LRO will use a repeating stationkeeping cycle with a pair of maneuvers every lunar sidereal period. The stationkeeping algorithm will bound LRO altitude, maintain ground station contact during maneuvers, and equally distribute periselene between northern and southern hemispheres. Orbit determination for LRO will be at the 50 m level with updated lunar gravity models. This paper will address the quasi-frozen orbit design, stationkeeping algorithms and low lunar orbit determination. INTRODUCTION The Lunar Reconnaissance Orbiter (LRO) is the first of the Lunar Precursor Robotic Program’s (LPRP) missions to the moon.
    [Show full text]
  • Educator's Guide: Orion
    Legends of the Night Sky Orion Educator’s Guide Grades K - 8 Written By: Dr. Phil Wymer, Ph.D. & Art Klinger Legends of the Night Sky: Orion Educator’s Guide Table of Contents Introduction………………………………………………………………....3 Constellations; General Overview……………………………………..4 Orion…………………………………………………………………………..22 Scorpius……………………………………………………………………….36 Canis Major…………………………………………………………………..45 Canis Minor…………………………………………………………………..52 Lesson Plans………………………………………………………………….56 Coloring Book…………………………………………………………………….….57 Hand Angles……………………………………………………………………….…64 Constellation Research..…………………………………………………….……71 When and Where to View Orion…………………………………….……..…77 Angles For Locating Orion..…………………………………………...……….78 Overhead Projector Punch Out of Orion……………………………………82 Where on Earth is: Thrace, Lemnos, and Crete?.............................83 Appendix………………………………………………………………………86 Copyright©2003, Audio Visual Imagineering, Inc. 2 Legends of the Night Sky: Orion Educator’s Guide Introduction It is our belief that “Legends of the Night sky: Orion” is the best multi-grade (K – 8), multi-disciplinary education package on the market today. It consists of a humorous 24-minute show and educator’s package. The Orion Educator’s Guide is designed for Planetarians, Teachers, and parents. The information is researched, organized, and laid out so that the educator need not spend hours coming up with lesson plans or labs. This has already been accomplished by certified educators. The guide is written to alleviate the fear of space and the night sky (that many elementary and middle school teachers have) when it comes to that section of the science lesson plan. It is an excellent tool that allows the parents to be a part of the learning experience. The guide is devised in such a way that there are plenty of visuals to assist the educator and student in finding the Winter constellations.
    [Show full text]
  • CCD Astrometry of the Host Star System HD 75289 with Exoplanet
    Vol. 15 No. 1 January 1, 2019 Journal of Double Star Observations Page 184 CCD Astrometry of the Host Star System HD 75289 with Exoplanet Charize C. Balignasay1,2, Jocelynn F. Bolosan1,2, Vea Aubrey Bumatay1,2, Pink Mariz G. Felipe1,2, Jeffrey Friedman3, Shanti C. Mohanan1,2, Donald C. Napala1,2, Skecynyth H. Perlas1,2, Vanessa Rhea C. Sao1,2, Evan Sugayama1,2, Lea Stuart3, Sierra Ryden3, Yasmina Vafaie3, Mark Silliman2, Brandi Giese 1, Kakkala Mohanan1, Diana Castaneda4, ,James D. Armstrong5, and Russell Genet6 1. University of Hawaii, Leeward Community College, Oahu, Hawaii 2. Waipahu High School Early College, Oahu, Hawaii 3. Montessori School of Maui, Maui, Hawaii 4. University of Hawaii at Manoa, Oahu, Hawaii 5. University of Hawaii Institute for Astronomy, Maui, Hawaii 6. California Polytechnic State University, San Luis Obispo, California Abstract: Student teams from the Early College Program in Oahu and the Montessori School of the Maui Work and Service Program made remote CCD measurements of a southern neglected double stars system HD 75289 using the Las Cumbres Observatory (LCO) global telescope network. The differential magnitude between primary and secondary was 6.7 requir- ing the use of z’ and Y filters for observation. While the primary is an F9, the exoplanet host- ing secondary is reported to be an M2. Astrometric solutions of the pair indicate a separation of 21.33 arcsec and a position angle of 76.99 degrees. termine theoretical orbits in a shorter time interval. Introduction A group of nine Early College Program students Gravitationally bound stellar objects obey Kepler’s from Waipahu High school located on the island of Oa- Laws of Motion.
    [Show full text]
  • September 2020 BRAS Newsletter
    A Neowise Comet 2020, photo by Ralf Rohner of Skypointer Photography Monthly Meeting September 14th at 7:00 PM, via Jitsi (Monthly meetings are on 2nd Mondays at Highland Road Park Observatory, temporarily during quarantine at meet.jit.si/BRASMeets). GUEST SPEAKER: NASA Michoud Assembly Facility Director, Robert Champion What's In This Issue? President’s Message Secretary's Summary Business Meeting Minutes Outreach Report Asteroid and Comet News Light Pollution Committee Report Globe at Night Member’s Corner –My Quest For A Dark Place, by Chris Carlton Astro-Photos by BRAS Members Messages from the HRPO REMOTE DISCUSSION Solar Viewing Plus Night Mercurian Elongation Spooky Sensation Great Martian Opposition Observing Notes: Aquila – The Eagle Like this newsletter? See PAST ISSUES online back to 2009 Visit us on Facebook – Baton Rouge Astronomical Society Baton Rouge Astronomical Society Newsletter, Night Visions Page 2 of 27 September 2020 President’s Message Welcome to September. You may have noticed that this newsletter is showing up a little bit later than usual, and it’s for good reason: release of the newsletter will now happen after the monthly business meeting so that we can have a chance to keep everybody up to date on the latest information. Sometimes, this will mean the newsletter shows up a couple of days late. But, the upshot is that you’ll now be able to see what we discussed at the recent business meeting and have time to digest it before our general meeting in case you want to give some feedback. Now that we’re on the new format, business meetings (and the oft neglected Light Pollution Committee Meeting), are going to start being open to all members of the club again by simply joining up in the respective chat rooms the Wednesday before the first Monday of the month—which I encourage people to do, especially if you have some ideas you want to see the club put into action.
    [Show full text]
  • A Low-Mass Stellar Companion of the Planet Host Star HD 75289
    A&A 425, 249–253 (2004) Astronomy DOI: 10.1051/0004-6361:20041009 & c ESO 2004 Astrophysics A low-mass stellar companion of the planet host star HD 75289 M. Mugrauer1, R. Neuhäuser1, T. Mazeh2,J.Alves3, and E. Guenther4 1 Astrophysikalisches Institut, Universität Jena, Schillergäßchen 2-3, 07745 Jena, Germany e-mail: [email protected] 2 Tel Aviv University, Tel Aviv 69978, Israel 3 European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching, Germany 4 Thüringer Landessternwarte Tautenburg, Sternwarte 5, 07778 Tautenburg, Germany Received 2 April 2004 / Accepted 3 June 2004 Abstract. We report on the detection of a new low-mass stellar companion of HD 75289, a G0V star that harbors one known radial-velocity planet (Udry et al. 2000, A&A, 356, 590). Comparing an image from 2MASS with an image we obtained with SofI at the ESO 3.58 m NTT three years later, we detected a co-moving companion located 21.465 ± 0.023 arcsec (621 ± 10 AU at 29 pc) east of HD 75289. A second SofI image taken 10 months later confirmed the common proper motion of HD 75289 B with its host star. The infrared spectrum and colors of the companion are consistent with an M 2 to M 5 main-sequence star at the distance of HD 75289. No further (sub)stellar companion down to H = 19 mag could be detected. With the SofI detection limit we can rule out additional stellar companions beyond 140 AU and substellar companions with masses m ≥ 0.050 M from 400 AU up to 2000 AU.
    [Show full text]
  • 2016 Publication Year 2021-04-23T14:32:39Z Acceptance in OA@INAF Age Consistency Between Exoplanet Hosts and Field Stars Title B
    Publication Year 2016 Acceptance in OA@INAF 2021-04-23T14:32:39Z Title Age consistency between exoplanet hosts and field stars Authors Bonfanti, A.; Ortolani, S.; NASCIMBENI, VALERIO DOI 10.1051/0004-6361/201527297 Handle http://hdl.handle.net/20.500.12386/30887 Journal ASTRONOMY & ASTROPHYSICS Number 585 A&A 585, A5 (2016) Astronomy DOI: 10.1051/0004-6361/201527297 & c ESO 2015 Astrophysics Age consistency between exoplanet hosts and field stars A. Bonfanti1;2, S. Ortolani1;2, and V. Nascimbeni2 1 Dipartimento di Fisica e Astronomia, Università degli Studi di Padova, Vicolo dell’Osservatorio 3, 35122 Padova, Italy e-mail: [email protected] 2 Osservatorio Astronomico di Padova, INAF, Vicolo dell’Osservatorio 5, 35122 Padova, Italy Received 2 September 2015 / Accepted 3 November 2015 ABSTRACT Context. Transiting planets around stars are discovered mostly through photometric surveys. Unlike radial velocity surveys, photo- metric surveys do not tend to target slow rotators, inactive or metal-rich stars. Nevertheless, we suspect that observational biases could also impact transiting-planet hosts. Aims. This paper aims to evaluate how selection effects reflect on the evolutionary stage of both a limited sample of transiting-planet host stars (TPH) and a wider sample of planet-hosting stars detected through radial velocity analysis. Then, thanks to uniform deriva- tion of stellar ages, a homogeneous comparison between exoplanet hosts and field star age distributions is developed. Methods. Stellar parameters have been computed through our custom-developed isochrone placement algorithm, according to Padova evolutionary models. The notable aspects of our algorithm include the treatment of element diffusion, activity checks in terms of 0 log RHK and v sin i, and the evaluation of the stellar evolutionary speed in the Hertzsprung-Russel diagram in order to better constrain age.
    [Show full text]