Human Vision and Dark Adaptation

Total Page:16

File Type:pdf, Size:1020Kb

Human Vision and Dark Adaptation AN ABSTRACT OF THE THESIS OF Carsten Christof Grellmann for the degree of Honors Baccalaureate of Science in Mechanical Engineering presented on May 22, 2009. Title: Light Pollution and the Limiting Visual Magnitude in Corvallis, Oregon. Abstract approved: Richard Peterson This study sought to ascertain the degree to which the night sky of Corvallis is affected by light pollution by determining the limiting visual magnitude. Defined as the brightness of the dimmest star that can be seen with the averted naked eye, the limiting visual magnitude establishes a quantitative standard by which to judge the quality of the night sky. Using the star count method and predetermined star fields prescribed by the International Meteor Organization, observations were conducted at Kings Boulevard and Van Buren Street, the Valley Library Quad, and Riverfront Park from the months of November to April. For the purposes of comparison, observations were also conducted at Adair County Park, downtown Portland, and Warm Springs in Central Oregon. This study concluded that the skies of Corvallis are moderately affected by light pollution, with limiting magnitudes between +5.85 and +6.27 with an uncertainty of ±0.12 for the three Corvallis sites, as compared to +7.16 at Warm Springs and +5.04 in downtown Portland. Furthermore, examples of light pollution and its effect on the night sky were photographically documented at each site with a Canon Digital Rebel XT camera and an 8-inch Schmidt-Cassegrain telescope. Key Words: Light Pollution, Limiting Visual Magnitude, Astronomy Corresponding email address: [email protected] ©Copyright by Carsten Christof Grellmann May 22, 2009 All Rights Reserved Light Pollution and the Limiting Visual Magnitude in Corvallis, Oregon By Carsten Christof Grellmann A PROJECT submitted to Oregon State University University Honors College in partial fulfillment of the requirements for the degree of Honors Baccalaureate of Science in Mechanical Engineering Presented May 22, 2009 Commencement June 2009 Honors Baccalaureate of Science in Mechanical Engineering project of Carsten C. Grellmann presented on May 22, 2009. APPROVED: Mentor, representing Mechanical, Industrial, and Manufacturing Engineering Committee Member, representing Physics Committee Member, representing Mechanical, Industrial, and Manufacturing Engineering Dean, University Honors College I understand that my project will become part of the permanent collection of Oregon State University, University Honors College. My signature below authorizes release of my project to any reader upon request. Carsten Christof Grellmann, Author Acknowledgements I would like to thank my mentor, Dr. Richard Peterson, and my committee members, Dr. Kenneth Krane, Dr. William Hetherington, and Dr. Nancy Squires, for serving as excellent resources and encouraging me in this research. Without their expertise and support, this project would not have been possible. I would also like to thank my parents for their support and encouragement in taking on this project, and the contributing members of the Excellence Fund, who generously provided $250 toward the purchase of a camera. Most of all, I would like to thank my sister, Elise Grellmann, for helping me carry my equipment around the city, and keeping me company on those long, cold nights of observing. Even though she irreverently calls star clusters “a bunch of sprinkles.” TABLE OF CONTENTS 1. INTRODUCTION .......................................................................................................... 1 2. BACKGROUND AND LITERATURE REVIEW ........................................................ 3 2.1. Light Pollution ......................................................................................................... 3 2.2. Limiting Visual Magnitude ...................................................................................... 6 2.3. Human Vision and Dark Adaptation ....................................................................... 8 2.4. Previous Star Counts .............................................................................................. 10 3. METHODS ................................................................................................................... 12 3.1. International Meteor Organization Star Count Method ......................................... 12 3.2. Observing Locations .............................................................................................. 14 3.3. Weather Conditions and the Moon ........................................................................ 19 3.4. Photographic Documentation ................................................................................ 19 4. RESULTS ..................................................................................................................... 22 4.1. Kings Boulevard and Van Buren Street ................................................................. 22 4.2. Valley Library Quad .............................................................................................. 24 4.3. Riverfront Park ...................................................................................................... 26 4.4. Adair County Park ................................................................................................. 28 4.5. Central Oregon ....................................................................................................... 28 4.6. Tom McCall Waterfront Park ................................................................................ 28 5. ANALYSIS ................................................................................................................... 29 5.1. Kings Boulevard and Van Buren Street ................................................................. 29 5.2. Valley Library Quad .............................................................................................. 32 5.3. Riverfront Park ...................................................................................................... 35 6. CONCLUSIONS........................................................................................................... 38 BIBLIOGRAPHY ............................................................................................................. 39 APPENDIX A: INTERNATIONAL METEOR ORGANIZATION STAR FIELDS ...... 40 LIST OF FIGURES Figure 1: Light Output from a Street Lamp (Adapted from Macrobert, 1996) .................. 4 Figure 2: Nighttime Photograph of the Kings and Van Buren Observation Site .............. 15 Figure 3: Primary Sources of Illumination around Kings and Van Buren Site ................ 15 Figure 4: Nighttime Photograph of the Valley Library Quad Observation Site ............... 16 Figure 5: Characteristic Sources of Illumination around Valley Library Quad Site ........ 17 Figure 6: Nighttime Photograph of the Riverfront Park Observation Site ....................... 18 Figure 7: Characteristic Sources of Illumination around Riverfront Park Site ................. 18 Figure 8: Tripod Mounted Canon Digital Rebel XT ........................................................ 20 Figure 9: Schmidt-Cassegrain Telescope with Camera Body Mounted to Rear Cell ....... 20 Figure 10: Focal Reducer, T-Adapter, T-Ring, and Camera Mounted to Telescope ........ 21 Figure 11: 10 s, 20 s, and 30 s Exposures of M35 from Kings and Van Buren ............... 23 Figure 12: 10 s, 20 s, and 30 s Exposures of M35 from the Valley Library Quad ........... 25 Figure 13: Limiting Visual Magnitude for Three Corvallis Locations for Typical New Moon to Full Moon Cycle................................................................................................. 26 Figure 14: 10 s, 20 s, and 30 s Exposures of M35 from Riverfront Park ......................... 27 Figure 15: 5 Minute Exposures of Big Dipper Taken from Kings and Van Buren (Top) and Adair County Park (Bottom) ...................................................................................... 30 Figure 16: Ring Nebula photographed from Kings and Van Buren (Left) and Adair County Park (Right) .......................................................................................................... 31 Figure 17: 5 Minute Exposures of Big Dipper Taken at Library Quad (Top) and Adair County Park (Bottom) ....................................................................................................... 33 Figure 18: Ring Nebula Photographed from Valley Library Quad (Left) and Adair County Park (Right) .......................................................................................................... 34 Figure 19: 5 Minute Exposures of Big Dipper Taken From Riverfront Park (Top) and Warm Springs (Bottom) .................................................................................................... 36 Figure 20: Ring Nebula Photographed from Riverfront Park (Left) and Adair County Park (Right) ....................................................................................................................... 37 1. INTRODUCTION Associated with poorly designed or improperly aimed outdoor lighting in urban areas, light pollution has gone from a local nuisance to a global problem in the one hundred years since the advent of the electric light bulb (Ploetz, 2002). As the nighttime glow of cities and suburban areas has increased, the nearly 7000 stars once visible to the naked eye under pristine conditions has shrunk to approximately 25 of the brightest celestial objects in the most light polluted
Recommended publications
  • Naming the Extrasolar Planets
    Naming the extrasolar planets W. Lyra Max Planck Institute for Astronomy, K¨onigstuhl 17, 69177, Heidelberg, Germany [email protected] Abstract and OGLE-TR-182 b, which does not help educators convey the message that these planets are quite similar to Jupiter. Extrasolar planets are not named and are referred to only In stark contrast, the sentence“planet Apollo is a gas giant by their assigned scientific designation. The reason given like Jupiter” is heavily - yet invisibly - coated with Coper- by the IAU to not name the planets is that it is consid- nicanism. ered impractical as planets are expected to be common. I One reason given by the IAU for not considering naming advance some reasons as to why this logic is flawed, and sug- the extrasolar planets is that it is a task deemed impractical. gest names for the 403 extrasolar planet candidates known One source is quoted as having said “if planets are found to as of Oct 2009. The names follow a scheme of association occur very frequently in the Universe, a system of individual with the constellation that the host star pertains to, and names for planets might well rapidly be found equally im- therefore are mostly drawn from Roman-Greek mythology. practicable as it is for stars, as planet discoveries progress.” Other mythologies may also be used given that a suitable 1. This leads to a second argument. It is indeed impractical association is established. to name all stars. But some stars are named nonetheless. In fact, all other classes of astronomical bodies are named.
    [Show full text]
  • GLOBE at Night: Using Sky Quality Meters to Measure Sky Brightness
    GLOBE at Night: using Sky Quality Meters to measure sky brightness This document includes: • How to observe with the SQM o The SQM, finding latitude and longitude, when to observe, taking and reporting measurements, what do the numbers mean, comparing results • Demonstrating light pollution o Background in light pollution and lighting, materials needed for the shielding demo, doing the shielding demo • Capstone activities (and resources) • Appendix: An excel file for multiple measurements CREDITS This document on citizen-scientists using Sky Quality Meters to monitor light pollution levels in their community was a collaborative effort between Connie Walker at the National Optical Astronomy Observatory, Chuck Bueter of nightwise.org, Anna Hurst of ASP’s Astronomy from the Ground Up program, Vivian White and Marni Berendsen of ASP’s Night Sky Network and Kim Patten of the International Dark-Sky Association. Observations using the Sky Quality Meter (SQM) The Sky Quality Meters (SQMs) add a new twist to the GLOBE at Night program. They expand the citizen science experience by making it more scientific and more precise. The SQMs allow citizen-scientists to map a city at different locations to identify dark sky oases and even measure changes over time beyond the GLOBE at Night campaign. This document outlines how to make and report SQM observations. Important parts of the SQM ! Push start button here. ! Light enters here. ! Read out numbers here. The SQM Model The SQM-L Model Using the SQM There are two models of Sky Quality Meters. Information on the newer model, the SQM- L, can be found along with the instruction sheet at http://unihedron.com/projects/sqm-l/.
    [Show full text]
  • SEPTEMBER 2014 OT H E D Ebn V E R S E R V ESEPTEMBERR 2014
    THE DENVER OBSERVER SEPTEMBER 2014 OT h e D eBn v e r S E R V ESEPTEMBERR 2014 FROM THE INSIDE LOOKING OUT Calendar Taken on July 25th in San Luis State Park near the Great Sand Dunes in Colorado, Jeff made this image of the Milky Way during an overnight camping stop on the way to Santa Fe, NM. It was taken with a Canon 2............................. First quarter moon 60D camera, an EFS 15-85 lens, using an iOptron SkyTracker. It is a single frame, with no stacking or dark/ 8.......................................... Full moon bias frames, at ISO 1600 for two minutes. Visible in this south-facing photograph is Sagittarius, and the 14............ Aldebaran 1.4˚ south of moon Dark Horse Nebula inside of the Milky Way. He processed the image in Adobe Lightroom. Image © Jeff Tropeano 15............................ Last quarter moon 22........................... Autumnal Equinox 24........................................ New moon Inside the Observer SEPTEMBER SKIES by Dennis Cochran ygnus the Swan dives onto center stage this other famous deep-sky object is the Veil Nebula, President’s Message....................... 2 C month, almost overhead. Leading the descent also known as the Cygnus Loop, a supernova rem- is the nose of the swan, the star known as nant so large that its separate arcs were known Society Directory.......................... 2 Albireo, a beautiful multi-colored double. One and named before it was found to be one wide Schedule of Events......................... 2 wonders if Albireo has any planets from which to wisp that came out of a single star. The Veil is see the pair up-close.
    [Show full text]
  • How to Make $1000 with Your Telescope! – 4 Stargazers' Diary
    Fort Worth Astronomical Society (Est. 1949) February 2010 : Astronomical League Member Club Calendar – 2 Opportunities & The Sky this Month – 3 How to Make $1000 with your Telescope! – 4 Astronaut Sally Ride to speak at UTA – 4 Aurgia the Charioteer – 5 Stargazers’ Diary – 6 Bode’s Galaxy by Steve Tuttle 1 February 2010 Sunday Monday Tuesday Wednesday Thursday Friday Saturday 1 2 3 4 5 6 Algol at Minima Last Qtr Moon Æ 5:48 am 11:07 pm Top ten binocular deep-sky objects for February: M35, M41, M46, M47, M50, M93, NGC 2244, NGC 2264, NGC 2301, NGC 2360 Top ten deep-sky objects for February: M35, M41, M46, M47, M50, M93, NGC 2261, NGC 2362, NGC 2392, NGC 2403 7 8 9 10 11 12 13 Algol at Minima Morning sports a Moon at Apogee New Moon Æ super thin crescent (252,612 miles) 8:51 am 7:56 pm Moon 8:00 pm 3RF Star Party Make use of the New Moon Weekend for . better viewing at the Dark Sky Site See Notes Below New Moon New Moon Weekend Weekend 14 15 16 17 18 19 20 Presidents Day 3RF Star Party Valentine’s Day FWAS Traveler’s Guide Meeting to the Planets UTA’s Maverick Clyde Tombaugh Ranger 8 returns Normal Room premiers on Speakers Series discovered Pluto photographs and NatGeo 7pm Sally Ride “Fat Tuesday” Ash Wednesday 80 years ago. impacts Moon. 21 22 23 24 25 26 27 Algol at Minima First Qtr Moon Moon at Perigee Å (222,345 miles) 6:42 pm 12:52 am 4 pm {Low in the NW) Algol at Minima Æ 9:43 pm Challenge binary star for month: 15 Lyncis (Lynx) Challenge deep-sky object for month: IC 443 (Gemini) Notable carbon star for month: BL Orionis (Orion) 28 Notes: Full Moon Look for a very thin waning crescent moon perched just above and slightly right of tiny Mercury on the morning of 10:38 pm Feb.
    [Show full text]
  • Sky Notes by Neil Bone 2005 August & September
    Sky notes by Neil Bone 2005 August & September below Castor and Pollux. Mercury is soon ing June and July, it is still quite possible that Sun and Moon lost from view again, arriving at superior con- noctilucent clouds (NLC) could be seen into junction beyond the Sun on September 18. early August, particularly by observers at The Sun continues its southerly progress along Venus continues its rather unfavourable more northerly locations. Quite how late into the ecliptic, reaching the autumnal equinox showing as an ‘Evening Star’. Although it August NLC can be seen remains to be deter- position at 22h 23m Universal Time (UT = pulls out to over 40° elongation east of the mined: there have been suggestions that the GMT; BST minus 1 hour) on September 22. Sun during September, Venus is also heading visibility period has become longer in recent At that precise time, the centre of the solar southwards, and as a result its setting-time years. Observational reports will be welcomed disk is positioned at the intersection between after the Sun remains much the same − barely by the Aurora Section. the celestial equator and the ecliptic, the latter an hour − during this interval. Although bright While declining sunspot activity makes great circle on the sky being inclined by 23.5° at magnitude −4, Venus will be quite tricky major aurorae extending to lower latitudes to the former. Calendrical autumn begins at the to catch in the early twilight: viewing cir- less likely, the appearance of coronal holes equinox, but amateur astronomers might more cumstances don’t really improve until the in the latter parts of the cycle does bring the readily follow meteorological timing, wherein closing weeks of 2005.
    [Show full text]
  • Measuring Night Sky Brightness: Methods and Challenges
    Measuring night sky brightness: methods and challenges Andreas H¨anel1, Thomas Posch2, Salvador J. Ribas3,4, Martin Aub´e5, Dan Duriscoe6, Andreas Jechow7,13, Zolt´anKollath8, Dorien E. Lolkema9, Chadwick Moore6, Norbert Schmidt10, Henk Spoelstra11, G¨unther Wuchterl12, and Christopher C. M. Kyba13,7 1Planetarium Osnabr¨uck,Klaus-Strick-Weg 10, D-49082 Osnabr¨uck,Germany 2Universit¨atWien, Institut f¨urAstrophysik, T¨urkenschanzstraße 17, 1180 Wien, Austria tel: +43 1 4277 53800, e-mail: [email protected] (corresponding author) 3Parc Astron`omicMontsec, Comarcal de la Noguera, Pg. Angel Guimer`a28-30, 25600 Balaguer, Lleida, Spain 4Institut de Ci`encies del Cosmos (ICCUB), Universitat de Barcelona, C.Mart´ıi Franqu´es 1, 08028 Barcelona, Spain 5D´epartement de physique, C´egep de Sherbrooke, Sherbrooke, Qu´ebec, J1E 4K1, Canada 6Formerly with US National Park Service, Natural Sounds & Night Skies Division, 1201 Oakridge Dr, Suite 100, Fort Collins, CO 80525, USA 7Leibniz-Institute of Freshwater Ecology and Inland Fisheries, 12587 Berlin, Germany 8E¨otv¨osLor´andUniversity, Savaria Department of Physics, K´arolyi G´asp´ar t´er4, 9700 Szombathely, Hungary 9National Institute for Public Health and the Environment, 3720 Bilthoven, The Netherlands 10DDQ Apps, Webservices, Project Management, Maastricht, The Netherlands 11LightPollutionMonitoring.Net, Urb. Ve¨ınatVerneda 101 (Bustia 49), 17244 Cass`ade la Selva, Girona, Spain 12Kuffner-Sternwarte,Johann-Staud-Straße 10, A-1160 Wien, Austria 13Deutsches GeoForschungsZentrum Potsdam, Telegrafenberg, 14473 Potsdam, Germany Abstract Measuring the brightness of the night sky has become an increasingly impor- tant topic in recent years, as artificial lights and their scattering by the Earth’s atmosphere continue spreading around the globe.
    [Show full text]
  • Sky & Telescope
    Eclipse from the See Sirius B: The Nearest Spot the Other EDGE OF SPACE p. 66 WHITE DWARF p. 30 BLUE PLANETS p. 50 THE ESSENTIAL GUIDE TO ASTRONOMY What Put the Bang in the Big Bang p. 22 Telescope Alignment Made Easy p. 64 Explore the Nearby Milky Way p. 32 How to Draw the Moon p. 54 OCTOBER 2013 Cosmic Gold Rush Racing to fi nd exploding stars p. 16 Visit SkyandTelescope.com Download Our Free SkyWeek App FC Oct2013_J.indd 1 8/2/13 2:47 PM “I can’t say when I’ve ever enjoyed owning anything more than my Tele Vue products.” — R.C, TX Tele Vue-76 Why Are Tele Vue Products So Good? Because We Aim to Please! For over 30-years we’ve created eyepieces and telescopes focusing on a singular target; deliver a cus- tomer experience “...even better than you imagined.” Eyepieces with wider, sharper fields of view so you see more at any power, Rich-field refractors with APO performance so you can enjoy Andromeda as well as Jupiter in all their splendor. Tele Vue products complement each other to pro- vide an observing experience as exquisite in performance as it is enjoyable and effortless. And how do we score with our valued customers? Judging by superlatives like: “in- credible, truly amazing, awesome, fantastic, beautiful, work of art, exceeded expectations by a mile, best quality available, WOW, outstanding, uncom- NP101 f/5.4 APO refractor promised, perfect, gorgeous” etc., BULLSEYE! See these superlatives in with 110° Ethos-SX eye- piece shown on their original warranty card context at TeleVue.com/comments.
    [Show full text]
  • CH02 End of Chapter Answers Review Questions 1. According To
    CH02 End of Chapter Answers Review Questions 1. According to Figure 2-7, the following wavelengths fall within the following ranges of the electromagnetic spectrum: a. 2.6 m – Infrared b. 34 m – Radio c. 0.54 nm – X-rays d. 0.0032 nm – Gamma rays e. 0.620 m – Visible f. 310 nm – Ultraviolet g. 0.012 m – This lies right near the border between microwave and radio waves. Since the figure is not accurate to two decimal places, it is not possible to determine within which wavelength regime this falls. 2. Since radio waves are a form of electromagnetic radiation, they travel at the speed of light. The wavelength and frequency of any wave is related by the formula: f = c, where c is equal to the speed of light, or 3 × 108 m/s. Using this formula, and knowing the values for both c and f (880.65 MHz, or 8.8065 × 108 Hz), we can solve for the wavelength: = 3 × 108 m/s / 8.8065 x 108 Hz = 0.341 meters. 3. According to the Stefan-Boltzmann law, hotter objects radiate more intensely than cooler objects. According to Wien’s law, that energy is not radiated uniformly at all wavelengths, but mostly at a wavelength that is inversely proportional to the temperature of the object. As a hot, glowing object becomes hotter, it radiates more intensely at all wavelengths, becoming brighter, and shifts the peak wavelength (at which it radiates the most energy) to shorter wavelengths, becoming bluer. 4. According to the Stefan-Boltzmann law, the intensity of a blackbody object is related to the temperature of an object to the fourth power.
    [Show full text]
  • CIRCULAR No. 170 (FEBRUARY 2010)
    INTERNATIONAL ASTRONOMICAL UNION COMMISSION 26 (DOUBLE STARS) INFORMATION CIRCULAR No. 170 (FEBRUARY 2010) NEW ORBITS ADS Name P T e ­(2000) 2010 Author(s) ®2000± n a i ! Last ob. 2011 111 BU 391 AB 616y04 2095.68 0.103 81±75 259±0 100352 ZIRM 00094-2759 0±5925 100500 98±98 256±86 2006.940 258.9 1.346 - SEE3 406.00 1978.45 0.850 267.70 117.00 0.801 HARTKOPF 00098-3347 0.8871 1.119 41.7 77.6 2008.5490 117.70 0.814 & MASON - HDS 33 29.03 2018.12 0.378 177.0 132.0 0.189 CVETKOVIC 00143-2732 12.4010 0.251 59.8 73.9 2008.5432 141.6 0.199 - B 1024 1466. 1926.38 0.814 126.0 73.1 0.410 LING 00149-3209 0.2456 1.586 110.4 311.8 2008.5431 72.3 0.410 238 A1803AB 35.66 1950.70 0.002 124.10 306.00 0.179 HARTKOPF 00174+0853 10.0950 0.189 95.4 282.0 2008.7670 305.00 0.187 & MASON 281 BU1015 137.00 1961.65 0.557 291.20 103.80 0.483 HARTKOPF 00206+1219 2.6283 0.333 35.0 10.0 2008.8879 104.70 0.487 & MASON - HDS 56 28.05 1999.30 0.481 96.1 294.0 0.326 CVETKOVIC 00251+4803 12.8323 0.230 164.0 358.9 2007.8257 288.7 0.334 - B1909 11.35 1995.09 0.005 119.49 311.90 0.175 HARTKOPF 00284-2020 31.7093 0.202 69.8 99.0 2009.6710 334.80 0.109 & MASON 475 D2AB 2981.00 2007.00 0.923 266.00 42.80 0.067 HARTKOPF 00345-0433 0.1208 2.740 77.5 80.2 2009.7560 55.40 0.090 & MASON 520 BU395 25.02 1998.78 0.218 291.98 96.70 0.496 HARTKOPF 00373-2446 14.3905 0.675 78.6 318.1 2009.7560 101.00 0.596 & MASON - I440 196.00 2142.00 0.650 57.00 269.30 0.402 HARTKOPF 00427-6537 1.8350 0.274 157.0 344.0 2009.6710 268.70 0.405 & MASON 1 NEW ORBITS (continuation) ADS Name P T e ­(2000) 2010 Author(s) ®2000± n a i ! Last ob.
    [Show full text]
  • A Model to Determine Naked-Eye Limiting Magnitude
    Volume 10 Issue 1 (2021) HS Research A Model to Determine Naked-Eye Limiting Magnitude Dasha Crocker1, Vincent Schmidt1 and Laura Schmidt1 1Bellbrook High School, Bellbrook, OH, USA ABSTRACT The purpose of this study was to determine which variables would be needed to generate a model that predicted the naked eye limiting magnitude on a given night. After background research was conducted, it seemed most likely that wind speed, air quality, skyglow, and cloud cover would contribute to the proposed model. This hypothesis was tested by obtaining local weather data, then determining the naked eye limiting magnitude for the local conditions. This procedure was repeated for the moon cycle of October, then repeated an additional 11 times in November, December, and January. After the initial 30 trials, r values were calculated for each variable that was measured. These values revealed that wind was not at all correlated with the naked eye limiting magnitude, but pollen (a measure of air quality), skyglow, and cloud cover were. After the generation of several models using multiple regression tests, air quality also proved not to affect the naked eye limiting magnitude. It was concluded that skyglow and cloud cover would contribute to a model that predicts naked eye limiting magnitude, proving the original hypothesis to be partially correct. Introduction Humanity has been looking to the stars for thousands of years. Ancient civilizations looked to the stars hoping that they could explain the world around them. Mayans invented shadow casting devices to track the movement of the sun, moon, and planets, while Chinese astronomers discovered Ganymede, one of Jupiter’s moons (Cook, 2018).
    [Show full text]
  • Binocular Universe: Aurigan Treasures
    Binocular Universe: Aurigan Treasures February 2012 Phil Harrington ead outside this evening and take a look high overhead. If you live in midnorthern latitudes, you will find a lone beacon cresting near the zenith as Hthe sky darkens. That's Capella, the Alpha (α) star of the constellation Auriga the Charioteer. Tracing back to ancient Rome, the name Capella translates as "She-Goat," a reference to the position it holds in the picture of the Charioteer. He is often portrayed as holding a goat and two kids in his arms. Above: Winter star map from Star Watch by Phil Harrington. Finder chart for this month's Binocular Universe, adapted from TUBA, www.philharrington.net/tuba.htm Today, we know that Capella is actually a binary star system lying some 42 light years away. Each of Capella's suns is classified as a type-G yellow star, like our Sun. That means that all three have roughly the same surface temperature, although our yellow dwarf Sun is only about one-tenth as large as either of the Capella giants. There is little hope of spotting the two Capella component stars through even the largest telescopes, since they are only separated by about 60 million miles, less than the distance from the Sun to Venus. The Charioteer’s pentagonal body highlights a wonderful area of the winter sky to scan with binoculars. There, you will find three of the season’s brightest open star clusters as well as an array of lesser known targets. M38, one of Auriga's three Messier open clusters, is centrally positioned within Auriga’s pentagonal body.
    [Show full text]
  • Extrasolar Planet Detection and Characterization with the KELT-North Transit Survey
    Extrasolar Planet Detection and Characterization With the KELT-North Transit Survey DISSERTATION Presented in Partial Fulfillment of the Requirements for the Degree Doctor of Philosophy in the Graduate School of The Ohio State University By Thomas G. Beatty Graduate Program in Astronomy The Ohio State University 2014 Dissertation Committee: Professor B. Scott Gaudi, Advisor Professor Andrew P. Gould Professor Marc H. Pinsonneault Copyright by Thomas G. Beatty 2014 Abstract My dissertation focuses on the detection and characterization of new transiting extrasolar planets from the KELT-North survey, along with a examination of the processes underlying the astrophysical errors in the type of radial velocity measurements necessary to measure exoplanetary masses. Since 2006, the KELT- North transit survey has been collecting wide-angle precision photometry for 20% of the sky using a set of target selection, lightcurve processing, and candidate identification protocols I developed over the winter of 2010-2011. Since our initial set of planet candidates were generated in April 2011, KELT-North has discovered seven new transiting planets, two of which are among the five brightest transiting hot Jupiter systems discovered via a ground-based photometric survey. This highlights one of the main goals of the KELT-North survey: to discover new transiting systems orbiting bright, V< 10, host stars. These systems offer us the best targets for the precision ground- and space-based follow-up observations necessary to measure exoplanetary atmospheres. In September 2012 I demonstrated the atmospheric science enabled by the new KELT planets by observing the secondary eclipses of the brown dwarf KELT-1b with the Spitzer Space Telescope.
    [Show full text]