FRAC 50 Observing List
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Art Matching
Art Matching Program Type: Demonstration or Classroom Audience Type: Grade 4–adult Program Description: Students explore how artists from different cultures have used art to represent space-related phenomena. Topics: Moon, space travel, art, stars, sky-watching Process Skills Focus: Critical thinking, observing, creativity. LEARNING OBJECTIVES For Next Generation Science Standards alignment, see end of outline. • Many artists are inspired by astronomy and the universe. • Cultures often have their own interpretations of the sky and celestial phenomena. • Art is one of many ways to capture our observations of and reflections on the sky. TIME REQUIRED Advance Prep Set Up Activity Clean Up 15 minutes 5 minutes 10 minutes 5 minutes SITE REQUIREMENTS • Table or other flat surface • Chairs (optional, but helpful for elderly or young audiences) Art Matching 1 Lenses on the Sky OMSI 2017 PROGRAM FORMAT Segment Format Time Introduction Large group discussion 2 min Art Matching Group Activity 5 min Wrap-Up Large group discussion 3 min SUPPLIES Permanent Supplies Amount Notes Laminated pages showing the artists 5 and their work Laminated cards showing 5 astronomical images ADVANCE PREPARATION • Print out, cut, and laminate the pages showing the artists and their work (at the end of the document). • Print out, cut, and laminate the five cards showing the astronomical images (at the end of the document). • Complete the activity to familiarize yourself with the process. SET UP Spread out the five pages showing the artists and their work on the table. Below the pages, place the five cards showing the astronomical objects. INTRODUCTION 2 minutes Let students speculate before offering answers to any questions. -
The HERACLES View of the H -To-HI Ratio in Galaxies
The HERACLES View of the H2-to-HI Ratio in Galaxies Adam Leroy (NRAO, Hubble Fellow) Fabian Walter, Frank Bigiel, the HERACLES and THINGS teams The Saturday Morning Summary • Star formation rate vs. gas relation on ~kpc scales breaks apart into: A relatively universal CO-SFR relation in nearby disks Systematic environmental scalings in the CO-to-HI ratio • The CO-to-HI ratio is a strong function of radius, total gas, and stellar surface density correlated with ISM properties: dust-to-gas ratio, pressure harder to link to dynamics: gravitational instability, arms • Interpretation: the CO-to-HI ratio traces the efficiency of GMC formation Density and dust can explain much of the observed behavior heracles Fabian Walter Erik Rosolowsky MPIA UBC Frank Bigiel Eva Schinnerer UC Berkeley THINGS plus… MPIA Elias Brinks Antonio Usero Gaelle Dumas U Hertfordshire OAN, Madrid MPIA Erwin de Blok Andreas Schruba Helmut Wiesemeyer U Cape Town IRAM … MPIA Rob Kennicutt Axel Weiss Karl Schuster Cambridge MPIfR IRAM Barry Madore Carsten Kramer Karin Sandstrom Carnegie IRAM MPIA Michele Thornley Daniela Calzetti Kelly Foyle Bucknell UMass MPIA Collaborators The HERA CO-Line Extragalactic Survey First maps Leroy et al. (2009) • IRAM 30m Large Program to map CO J = 2→1 line • Instrument: HERA receiver array operating at 230 GHz • 47 galaxies: dwarfs to starbursts and massive spirals -2 • Very wide-field (~ r25) and sensitive (σ ~ 1-2 Msun pc ) NGS The HI Nearby Galaxy Survey HI Walter et al. (2008), AJ Special Issue (2008) • VLA HI maps of 34 galaxies: -
Rosette Nebula and Monoceros Loop
Oshkosh Scholar Page 43 Studying Complex Star-Forming Fields: Rosette Nebula and Monoceros Loop Chris Hathaway and Anthony Kuchera, co-authors Dr. Nadia Kaltcheva, Physics and Astronomy, faculty adviser Christopher Hathaway obtained a B.S. in physics in 2007 and is currently pursuing his masters in physics education at UW Oshkosh. He collaborated with Dr. Nadia Kaltcheva on his senior research project and presented their findings at theAmerican Astronomical Society meeting (2008), the Celebration of Scholarship at UW Oshkosh (2009), and the National Conference on Undergraduate Research in La Crosse, Wisconsin (2009). Anthony Kuchera graduated from UW Oshkosh in May 2008 with a B.S. in physics. He collaborated with Dr. Kaltcheva from fall 2006 through graduation. He presented his astronomy-related research at Posters in the Rotunda (2007 and 2008), the Wisconsin Space Conference (2007), the UW System Symposium for Undergraduate Research and Creative Activity (2007 and 2008), and the American Astronomical Society’s 211th meeting (2008). In December 2009 he earned an M.S. in physics from Florida State University where he is currently working toward a Ph.D. in experimental nuclear physics. Dr. Nadia Kaltcheva is a professor of physics and astronomy. She received her Ph.D. from the University of Sofia in Bulgaria. She joined the UW Oshkosh Physics and Astronomy Department in 2001. Her research interests are in the field of stellar photometry and its application to the study of Galactic star-forming fields and the spiral structure of the Milky Way. Abstract An investigation that presents a new analysis of the structure of the Northern Monoceros field was recently completed at the Department of Physics andAstronomy at UW Oshkosh. -
Big Halpha Kinematical Sample of Barred Spiral Galaxies - I
BhaBAR: Big Halpha kinematical sample of BARred spiral galaxies - I. Fabry-Perot Observations of 21 galaxies O. Hernandez, C. Carignan, P. Amram, L. Chemin, O. Daigle To cite this version: O. Hernandez, C. Carignan, P. Amram, L. Chemin, O. Daigle. BhaBAR: Big Halpha kinematical sample of BARred spiral galaxies - I. Fabry-Perot Observations of 21 galaxies. Monthly Notices of the Royal Astronomical Society, Oxford University Press (OUP): Policy P - Oxford Open Option A, 2005, 360 Issue 4, pp.1201. 10.1111/j.1365-2966.2005.09125.x. hal-00014446 HAL Id: hal-00014446 https://hal.archives-ouvertes.fr/hal-00014446 Submitted on 26 Jan 2021 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. Mon. Not. R. Astron. Soc. 360, 1201–1230 (2005) doi:10.1111/j.1365-2966.2005.09125.x BHαBAR: big Hα kinematical sample of barred spiral galaxies – I. Fabry–Perot observations of 21 galaxies O. Hernandez,1,2 † C. Carignan,1 P. Amram,2 L. Chemin1 and O. Daigle1 1Observatoire du mont Megantic,´ LAE, Universitede´ Montreal,´ CP 6128 succ. centre ville, Montreal,´ Quebec,´ Canada H3C 3J7 2Observatoire Astronomique de Marseille Provence et LAM, 2 pl. -
Filter Performance Comparisons for Some Common Nebulae
Filter Performance Comparisons For Some Common Nebulae By Dave Knisely Light Pollution and various “nebula” filters have been around since the late 1970’s, and amateurs have been using them ever since to bring out detail (and even some objects) which were difficult to impossible to see before in modest apertures. When I started using them in the early 1980’s, specific information about which filter might work on a given object (or even whether certain filters were useful at all) was often hard to come by. Even those accounts that were available often had incomplete or inaccurate information. Getting some observational experience with the Lumicon line of filters helped, but there were still some unanswered questions. I wondered how the various filters would rank on- average against each other for a large number of objects, and whether there was a “best overall” filter. In particular, I also wondered if the much-maligned H-Beta filter was useful on more objects than the two or three targets most often mentioned in publications. In the summer of 1999, I decided to begin some more comprehensive observations to try and answer these questions and determine how to best use these filters overall. I formulated a basic survey covering a moderate number of emission and planetary nebulae to obtain some statistics on filter performance to try to address the following questions: 1. How do the various filter types compare as to what (on average) they show on a given nebula? 2. Is there one overall “best” nebula filter which will work on the largest number of objects? 3. -
Spatial and Kinematic Structure of Monoceros Star-Forming Region
MNRAS 476, 3160–3168 (2018) doi:10.1093/mnras/sty447 Advance Access publication 2018 February 22 Spatial and kinematic structure of Monoceros star-forming region M. T. Costado1‹ and E. J. Alfaro2 1Departamento de Didactica,´ Universidad de Cadiz,´ E-11519 Puerto Real, Cadiz,´ Spain. Downloaded from https://academic.oup.com/mnras/article-abstract/476/3/3160/4898067 by Universidad de Granada - Biblioteca user on 13 April 2020 2Instituto de Astrof´ısica de Andaluc´ıa, CSIC, Apdo 3004, E-18080 Granada, Spain Accepted 2018 February 9. Received 2018 February 8; in original form 2017 December 14 ABSTRACT The principal aim of this work is to study the velocity field in the Monoceros star-forming region using the radial velocity data available in the literature, as well as astrometric data from the Gaia first release. This region is a large star-forming complex formed by two associations named Monoceros OB1 and OB2. We have collected radial velocity data for more than 400 stars in the area of 8 × 12 deg2 and distance for more than 200 objects. We apply a clustering analysis in the subspace of the phase space formed by angular coordinates and radial velocity or distance data using the Spectrum of Kinematic Grouping methodology. We found four and three spatial groupings in radial velocity and distance variables, respectively, corresponding to the Local arm, the central clusters forming the associations and the Perseus arm, respectively. Key words: techniques: radial velocities – astronomical data bases: miscellaneous – parallaxes – stars: formation – stars: kinematics and dynamics – open clusters and associations: general. Hoogerwerf & De Bruijne 1999;Lee&Chen2005; Lombardi, 1 INTRODUCTION Alves & Lada 2011). -
Winter Constellations
Winter Constellations *Orion *Canis Major *Monoceros *Canis Minor *Gemini *Auriga *Taurus *Eradinus *Lepus *Monoceros *Cancer *Lynx *Ursa Major *Ursa Minor *Draco *Camelopardalis *Cassiopeia *Cepheus *Andromeda *Perseus *Lacerta *Pegasus *Triangulum *Aries *Pisces *Cetus *Leo (rising) *Hydra (rising) *Canes Venatici (rising) Orion--Myth: Orion, the great hunter. In one myth, Orion boasted he would kill all the wild animals on the earth. But, the earth goddess Gaia, who was the protector of all animals, produced a gigantic scorpion, whose body was so heavily encased that Orion was unable to pierce through the armour, and was himself stung to death. His companion Artemis was greatly saddened and arranged for Orion to be immortalised among the stars. Scorpius, the scorpion, was placed on the opposite side of the sky so that Orion would never be hurt by it again. To this day, Orion is never seen in the sky at the same time as Scorpius. DSO’s ● ***M42 “Orion Nebula” (Neb) with Trapezium A stellar nursery where new stars are being born, perhaps a thousand stars. These are immense clouds of interstellar gas and dust collapse inward to form stars, mainly of ionized hydrogen which gives off the red glow so dominant, and also ionized greenish oxygen gas. The youngest stars may be less than 300,000 years old, even as young as 10,000 years old (compared to the Sun, 4.6 billion years old). 1300 ly. 1 ● *M43--(Neb) “De Marin’s Nebula” The star-forming “comma-shaped” region connected to the Orion Nebula. ● *M78--(Neb) Hard to see. A star-forming region connected to the Orion Nebula. -
Luminous Blue Variables
Review Luminous Blue Variables Kerstin Weis 1* and Dominik J. Bomans 1,2,3 1 Astronomical Institute, Faculty for Physics and Astronomy, Ruhr University Bochum, 44801 Bochum, Germany 2 Department Plasmas with Complex Interactions, Ruhr University Bochum, 44801 Bochum, Germany 3 Ruhr Astroparticle and Plasma Physics (RAPP) Center, 44801 Bochum, Germany Received: 29 October 2019; Accepted: 18 February 2020; Published: 29 February 2020 Abstract: Luminous Blue Variables are massive evolved stars, here we introduce this outstanding class of objects. Described are the specific characteristics, the evolutionary state and what they are connected to other phases and types of massive stars. Our current knowledge of LBVs is limited by the fact that in comparison to other stellar classes and phases only a few “true” LBVs are known. This results from the lack of a unique, fast and always reliable identification scheme for LBVs. It literally takes time to get a true classification of a LBV. In addition the short duration of the LBV phase makes it even harder to catch and identify a star as LBV. We summarize here what is known so far, give an overview of the LBV population and the list of LBV host galaxies. LBV are clearly an important and still not fully understood phase in the live of (very) massive stars, especially due to the large and time variable mass loss during the LBV phase. We like to emphasize again the problem how to clearly identify LBV and that there are more than just one type of LBVs: The giant eruption LBVs or h Car analogs and the S Dor cycle LBVs. -
CCD UBV Photometry and Kinematics of the Open Cluster NGC
CCD UBV Photometry and Kinematics of the Open Cluster NGC 225 Sel¸cuk Bilira,∗, Z. Funda Bostancıa, Talar Yontanb, Tolga G¨uvera, Volkan Bakı¸sc, Tansel Aka, Serap Aka, Ernst Paunzend, Zeki Ekerc aIstanbul University, Faculty of Science, Department of Astronomy and Space Sciences, 34119 University, Istanbul, Turkey bIstanbul University, Graduate School of Science and Engineering, Department of Astronomy and Space Sciences, 34116, Beyazıt, Istanbul, Turkey cDepartment of Space Sciences and Technologies, Faculty of Sciences, Akdeniz University, Antalya 07058, Turkey dDepartment of Theoretical Physics and Astrophysics, Masaryk University, Kotl´a˘rsk´a2, 611 37 Brno, Czech Republic Abstract We present the results of CCD UBV photometric and spectroscopic obser- vations of the open cluster NGC 225. In order to determine the structural parameters of NGC 225, we calculated the stellar density profile in the clus- ter’s field. We estimated the probabilities of the stars being physical members of the cluster using the existing astrometric data. The most likely members of the cluster were used in the determination of the astrophysical parame- ters of the cluster. We calculated the mean radial velocity of the cluster as −1 Vr = 8.3 5.0 km s from the optical spectra of eight stars in the cluster’s field.− Using± the U B vs B V two-colour diagram and UV excesses of the F- − − G type main-sequence stars, the reddening and metallicity of NGC 225 were inferred as E(B V )=0.151 0.047 mag and [Fe/H]= 0.11 0.01 dex, respectively. We− fitted the colour-magnitude± diagrams of NGC− 225± with the arXiv:1606.08608v1 [astro-ph.GA] 28 Jun 2016 PARSEC isochrones and derived the distance modulus, distance and age of the cluster as µ =9.3 0.07 mag, d = 585 20 pc and t = 900 100 Myr, V ± ± ± respectively. -
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. -
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. -
Feb BACK BAY 2019
Feb BACK BAY 2019 The official newsletter of the Back Bay Amateur Astronomers CONTENTS COMING UP Gamma Burst 2 Feb 7 BBAA Meeting Eclipse Collage 3 7:30-9PM TCC, Virginia Beach NSN Article 6 Heart Nebula 7 Feb 8 Silent Sky Club meeting 10 10-11PM Little Theatre of VB Winter DSOs 11 Contact info 16 Feb 8 Cornwatch Photo by Chuck Jagow Canon 60Da, various exposures, iOptron mount with an Orion 80ED Calendar 17 dusk-dawn The best 9 out of 3465 images taken from about 10:00 PM on the 20th Cornland Park through 2:20 AM on the 21st. Unprocessed images (only cropped). Feb 14 Garden Stars 7-8:30PM LOOKING UP! a message from the president Norfolk Botanical Gardens This month’s most talked about astronomy event has to be the total lunar Feb 16 Saturday Sun-day eclipse. The BBAA participated by supporting the Watch Party at the 10AM-1PM Chesapeake Planetarium. Anyone in attendance will tell you it was COLD, but Elizabeth River Park manageable if you wore layers, utilized the planetarium where Dr. Robert Hitt seemed to have the thermostat set to 100 degrees, and drank copious amounts Feb 23 Skywatch of the hot coffee that Kent Blackwell brewed in the back office. 6PM-10PM The event had a huge following on Facebook but with the cold Northwest River Park temperatures, we weren’t sure how many would come out. By Kent’s estimate there were between 100–200 people in attendance. Many club members set up telescopes, as well as a few members of the public too.