Deep Sky Objects
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Ray Emission from the Globular Cluster 47 Tucanae (Research Note)
A&A 499, 273–277 (2009) Astronomy DOI: 10.1051/0004-6361/200811564 & c ESO 2009 Astrophysics HESS upper limit on the very high energy γ-ray emission from the globular cluster 47 Tucanae (Research Note) F. Aharonian1,2, A. G. Akhperjanian3,G.Anton4, U. Barres de Almeida5,, A. R. Bazer-Bachi6, Y. Becherini7, B. Behera8, K. Bernlöhr1,9, C. Boisson10, A. Bochow1, V. Borrel6,I.Braun1,E.Brion11, J. Brucker4,P.Brun11, R. Bühler1,T.Bulik12, I. Büsching13, T. Boutelier14,P.M.Chadwick5, A. Charbonnier15,R.C.G.Chaves1, A. Cheesebrough5, L.-M. Chounet16,A.C.Clapson1, G. Coignet17, M. Dalton9,M.K.Daniel5,I.D.Davids18,13, B. Degrange16,C.Deil1, H. J. Dickinson5, A. Djannati-Ataï7, W. Domainko1, L. O’C. Drury2, F. Dubois17, G. Dubus14, J. Dyks12, M. Dyrda19,K.Egberts1, D. Emmanoulopoulos8, P. Espigat7, C. Farnier20, F. Feinstein20, A. Fiasson20, A. Förster1, G. Fontaine16,M.Füßling9,S.Gabici2,Y.A.Gallant20,L.Gérard7, B. Giebels16, J. F. Glicenstein11, B. Glück4,P.Goret11, D. Hauser8, M. Hauser8,S.Heinz4, G. Heinzelmann21,G.Henri14,G.Hermann1,J.A.Hinton22, A. Hoffmann23, W. Hofmann1, M. Holleran13, S. Hoppe1,D.Horns21, A. Jacholkowska15, O. C. de Jager13, I. Jung4, K. Katarzynski´ 24,U.Katz4, S. Kaufmann8, E. Kendziorra23, M. Kerschhaggl9, D. Khangulyan1, B. Khélifi16,D. Keogh5,Nu.Komin11, K. Kosack1,G.Lamanna17,J.-P.Lenain10, T. Lohse9, V. Marandon7, J. M. Martin10, O. Martineau-Huynh15 , A. Marcowith20, D. Maurin15,T.J.L.McComb5,M.C.Medina10, R. Moderski12, E. Moulin11, M. Naumann-Godo16, M. de Naurois15, D. Nedbal25, D. -
Unusual Orbits in the Andromeda Galaxy Post-16
Unusual orbits in the Andromeda galaxy Post-16 Topics covered: spectra, Doppler effect, Newton’s law of gravitation, galaxy rotation curves, arc lengths, cosmological units, dark matter Teacher’s Notes In this activity students will use real scientific data to plot the rotation curve of M31 (Andromeda), our neighbouring spiral galaxy. They will use Kepler’s third law to predict the motion of stars around the centre of M31. They will then measure the wavelengths of hydrogen emission spectra taken at a range of radii. The Doppler equation will be used to determine whether these spectra come from the approaching or receding limb of the galaxy and the velocity of rotation at that point. They will plot a velocity vs radius graph and compare it with their predicted result. A flat rotation curve indicates the presence of dark matter within Andromeda. Equipment: calculator, ruler, graph paper (if needed) Questions to ask the class before the activity: What is the Universe composed of? Answer: energy, luminous matter, dark matter, dark energy. What is a spectrum and how so we get spectral lines? Answer: a ‘fingerprint’ of an object made of light. The spectrum of visible light is composed of the colours of the rainbow. Absorption lines arise from electrons absorbing photons of light and jumping an energy level or levels; emission lines occur when electrons fall down to a lower energy level and emit a photon in the process. What can a spectrum tell us? Answer: the composition of an object such as a star, its temperature, its pressure, the abundance of elements in the star, its motion (velocity). -
Messier Objects
Messier Objects From the Stocker Astroscience Center at Florida International University Miami Florida The Messier Project Main contributors: • Daniel Puentes • Steven Revesz • Bobby Martinez Charles Messier • Gabriel Salazar • Riya Gandhi • Dr. James Webb – Director, Stocker Astroscience center • All images reduced and combined using MIRA image processing software. (Mirametrics) What are Messier Objects? • Messier objects are a list of astronomical sources compiled by Charles Messier, an 18th and early 19th century astronomer. He created a list of distracting objects to avoid while comet hunting. This list now contains over 110 objects, many of which are the most famous astronomical bodies known. The list contains planetary nebula, star clusters, and other galaxies. - Bobby Martinez The Telescope The telescope used to take these images is an Astronomical Consultants and Equipment (ACE) 24- inch (0.61-meter) Ritchey-Chretien reflecting telescope. It has a focal ratio of F6.2 and is supported on a structure independent of the building that houses it. It is equipped with a Finger Lakes 1kx1k CCD camera cooled to -30o C at the Cassegrain focus. It is equipped with dual filter wheels, the first containing UBVRI scientific filters and the second RGBL color filters. Messier 1 Found 6,500 light years away in the constellation of Taurus, the Crab Nebula (known as M1) is a supernova remnant. The original supernova that formed the crab nebula was observed by Chinese, Japanese and Arab astronomers in 1054 AD as an incredibly bright “Guest star” which was visible for over twenty-two months. The supernova that produced the Crab Nebula is thought to have been an evolved star roughly ten times more massive than the Sun. -
Adrienne M. Cool CURRICULUM VITAE Department
Adrienne M. Cool CURRICULUM VITAE Department of Physics and Astronomy San Francisco State University Tel: (415)338-6450 1600 Holloway Avenue Fax: (415)338-2178 San Francisco, CA 94132 E-mail: [email protected] Education Ph.D. Astronomy, Harvard University (1994) M.S. Electrical Engineering, Columbia University (1986) B.S. Physics, Yale University (1984) Employment 2006–present Professor, Department of Physics and Astronomy San Francisco State University 2000–06 Associate Professor, Department of Physics and Astronomy San Francisco State University 1996–00 Assistant Professor, Department of Physics and Astronomy San Francisco State University 1993–96 Postdoctoral Researcher, Department of Astronomy University of California, Berkeley 1988–93 Research Assistant, Department of Astronomy Harvard University 1988–90 Teaching Assistant, Department of Astronomy Harvard University 1987 Research Assistant, Astrophysics Laboratory Columbia University 1986 Teaching Assistant, Department of Electrical Engineering Columbia University 1985 Research Assistant, Department of Electrical Engineering Columbia University 1984 Private instructor in mathematics and physics 1981–84 Technical Assistant, Department of Nuclear Medicine Mount Sinai Medical Center, New York City Honors and Awards • Image of globular star cluster Omega Centauri chosen for Hubble Heritage web site (2008) • Affirmative Action Award, San Francisco State University (2005) • Image of globular star cluster NGC 6397 chosen for Hubble Heritage web site (2003) • Presidential Award for Professional Development of Probationary Faculty, San Francisco State University (2000) 1 • Outstanding Contributions to Teaching Certificate, San Francisco State University (1997) • Fellow, NASA Graduate Student Researchers Program (1992-93) • Harvard Merit Fellowship (1990) • Danforth Center Certificate for Teaching Excellence, Harvard University (1989) • Amelia Earhart Fellowship Award, Zonta International Foundation (1989, 1990) • Teaching Assistant/Scholar Award, Columbia University, Dept. -
Report of Contributions
Mapping the X-ray Sky with SRG: First Results from eROSITA and ART-XC Report of Contributions https://events.mpe.mpg.de/e/SRG2020 Mapping the X- … / Report of Contributions eROSITA discovery of a new AGN … Contribution ID : 4 Type : Oral Presentation eROSITA discovery of a new AGN state in 1H0707-495 Tuesday, 17 March 2020 17:45 (15) One of the most prominent AGNs, the ultrasoft Narrow-Line Seyfert 1 Galaxy 1H0707-495, has been observed with eROSITA as one of the first CAL/PV observations on October 13, 2019 for about 60.000 seconds. 1H 0707-495 is a highly variable AGN, with a complex, steep X-ray spectrum, which has been the subject of intense study with XMM-Newton in the past. 1H0707-495 entered an historical low hard flux state, first detected with eROSITA, never seen before in the 20 years of XMM-Newton observations. In addition ultra-soft emission with a variability factor of about 100 has been detected for the first time in the eROSITA light curves. We discuss fast spectral transitions between the cool and a hot phase of the accretion flow in the very strong GR regime as a physical model for 1H0707-495, and provide tests on previously discussed models. Presenter status Senior eROSITA consortium member Primary author(s) : Prof. BOLLER, Thomas (MPE); Prof. NANDRA, Kirpal (MPE Garching); Dr LIU, Teng (MPE Garching); MERLONI, Andrea; Dr DAUSER, Thomas (FAU Nürnberg); Dr RAU, Arne (MPE Garching); Dr BUCHNER, Johannes (MPE); Dr FREYBERG, Michael (MPE) Presenter(s) : Prof. BOLLER, Thomas (MPE) Session Classification : AGN physics, variability, clustering October 3, 2021 Page 1 Mapping the X- … / Report of Contributions X-ray emission from warm-hot int … Contribution ID : 9 Type : Poster X-ray emission from warm-hot intergalactic medium: the role of resonantly scattered cosmic X-ray background We revisit calculations of the X-ray emission from warm-hot intergalactic medium (WHIM) with particular focus on contribution from the resonantly scattered cosmic X-ray background (CXB). -
Research Investigates the Brightest Star of 47 Tucanae 10 August 2021, by Tomasz Nowakowski
Research investigates the brightest star of 47 Tucanae 10 August 2021, by Tomasz Nowakowski The brightest star of 47 Tuc at both ultraviolet and optical wavelengths is the so-called "Bright Star" (BS). It is a blue giant star of spectral type B8 III with an effective temperature of some 11,000 K. Moreover, the Bright Star is a post-asymptotic giant branch (post-AGB) star that is moving across the color-magnitude diagram toward the tip of the white- dwarf cooling sequence. Although many studies of the bright star have been conducted, its chemical composition is still poorly understood. Given that the Bright Star represents a unique window into the chemistry of 47 Tuc, a team of astronomers led by William V. Dixon of the Space Telescope Science Institute in Baltimore, Globular cluster 47 Tucanae. Credit: NASA, ESA, and Maryland, investigated this star using the Far the Hubble Heritage (STScI/AURA)-ESA/Hubble Ultraviolet Spectroscopic Explorer (FUSE), the Collaboration. Hubble Space Telescope (HST) and the Magellan Telescope. The observations allowed the team to determine Astronomers have inspected the brightest star of a photospheric abundances of 26 elements of the globular cluster known as 47 Tucanae (other bright star. The data show that the intermediate- designation NGC 104). Results of the study, mass elements generally scale with iron, while the published August 3 on arXiv.org, provide important heaviest elements have roughly solar abundances. insights into the properties and chemical It was found that the star has a relatively low composition of this star, what could improve our carbon to nitrogen ratio, what suggests that it understanding of the cluster's nature. -
Preliminary Catalogue of Isaac Roberts's Collection of Photographs of Celestial Objects
ASTRONOMISCHE NACHRICHTEN. Nr. 4154. Band 174. 2. Preliminary catalogue of Isaac Roberts’s collection of photographs of celestial objects. By Dorotha Isaac-Roberts. The Isaac Roberts collection of celestial photographs The number of the copies of the forthcoming paper comprises 2485 original negatives of stars, star-clusters, being very limited, the observatories and astronomers, official nebulae and other celestial objects together with many posi. or amateur, who are specially interested in photographic tives on glass and on paper, taken by the late Dr. Isaac astronomy will please send in their names to the address Roberts or, under his incessant supervision, by his assistant given below, early in 1907, in order that the various parts W. S. Franks, F. R. A. S., at Dr. Roberts’s Private Obser- of the complete catalogue may be sent to them in course vatory, Kennessee, Maghull, near Liverpool (1885-1 890) and, of time. from 1890 to 1904, at Starfield, Crowborough, Sussex. Positives- on-glass reproduced from the Isaac Roberts Of the above mentioned negatives, negatives will be lent for the purpose of micrometric mea- I) 1412 were taken with the zo-in Reflector (focal surements, if, application be made and provided that the length = 98.0 ins) and with an exposure of the plate of documents be returned after completion of the measurements. ninety minutes in general. In the preliminary catalogue given below, the numbers 2) 648 with the 5-in Cooke lens (f. 1. = 19.22 ins) of Dr. Dreyer’s New General Catalogue of Nebulae and which was mounted on the tube of the zo-in Reflector; or, Clusters of Stars and of Dr. -
Facilitator Information – Galaxies
Facilitator Information (All you need to know about galaxies to survive the day) What is a galaxy? Galaxies are large collections of stars and gas and dust. They have millions to billions of stars, all held into a cluster by gravitational attraction. Most galaxies are flat, but there are different shapes — some are spirals, some are elliptical, and some are irregular. Our Galaxy The Milky Way is a galaxy, a slowly rotating cluster of more than 200,000,000,000 stars! Our Milky Way Galaxy looks a little like a pinwheel. It is a spiral galaxy, about 100,000 light years across. Spiral galaxies have: a bulge in the center (called the nuclear bulge) that contains the nucleus; a wide, flat disk with distinct spiral arms containing stars; and a surrounding halo of stars. There are several “spiral arms” in our Milky Way: Sagittarius, Cygnus, Perseus, and Orion. Where are we in the Milky Way Galaxy? We are in one of the spiral arms, about 30,000 light years from the center of the Milky Way Galaxy — or about two-thirds of the way from the center. Can you see the Milky Way? Yes! On a very dark night, away from bright lights, you can see a faint, hazy — or milky — band in the sky. This is the Milky Way. The hazy appearance is because there so many stars that are very distant; your eye cannot distinguish the stars as separate points of light. By using binoculars or a telescope, you can see the individual stars. The Milky Way is like a big, flat disk in space. -
The Andromeda Galaxy's Most Important Merger
The Andromeda Galaxy’s most important merger ~ 2 Gyrs ago as M32’s likely progenitor Richard D’Souza* & Eric F. Bell Although the Andromeda Galaxy’s (M31) proximity offers a singular opportunity to understand how mergers affect galaxies1, uncertainty remains about M31’s most important mergers. Previous studies focused individually on the giant stellar stream2 or the impact of M32 on M31’s disk3,4, thereby suggesting many significant satellite interactions5. Yet, models of M31’s disk heating6 and the similarity between the stellar populations of different tidal substructures in M31’s outskirts7 both suggested a single large merger. M31’s outer low- surface brightness regions (its stellar halo) is built up from the tidal debris of satellites5 and provides decisive guidance about its important mergers8. Here we use cosmological models of galaxy formation9,10 to show that M31’s massive11 and metal-rich12 stellar halo, containing intermediate-age stars7, dramatically narrows the range of allowed interactions, requiring a 10 single dominant merger with a large galaxy (M*~2.5x10 M¤, the third largest member of the Local Group) ~2 Gyr ago. This single event explains many observations that were previously considered separately: its compact and metal-rich satellite M3213 is likely to be the stripped core of the disrupted galaxy, M31’s rotating inner stellar halo14 contains most of the merger debris, and the giant stellar stream15 is likely to have been thrown out during the merger. This interaction may explain M31’s global burst of star formation ~2 Gyr ago16 in which ~1/5 of its stars were formed. -
Nd AAS Meeting Abstracts
nd AAS Meeting Abstracts 101 – Kavli Foundation Lectureship: The Outreach Kepler Mission: Exoplanets and Astrophysics Search for Habitable Worlds 200 – SPD Harvey Prize Lecture: Modeling 301 – Bridging Laboratory and Astrophysics: 102 – Bridging Laboratory and Astrophysics: Solar Eruptions: Where Do We Stand? Planetary Atoms 201 – Astronomy Education & Public 302 – Extrasolar Planets & Tools 103 – Cosmology and Associated Topics Outreach 303 – Outer Limits of the Milky Way III: 104 – University of Arizona Astronomy Club 202 – Bridging Laboratory and Astrophysics: Mapping Galactic Structure in Stars and Dust 105 – WIYN Observatory - Building on the Dust and Ices 304 – Stars, Cool Dwarfs, and Brown Dwarfs Past, Looking to the Future: Groundbreaking 203 – Outer Limits of the Milky Way I: 305 – Recent Advances in Our Understanding Science and Education Overview and Theories of Galactic Structure of Star Formation 106 – SPD Hale Prize Lecture: Twisting and 204 – WIYN Observatory - Building on the 308 – Bridging Laboratory and Astrophysics: Writhing with George Ellery Hale Past, Looking to the Future: Partnerships Nuclear 108 – Astronomy Education: Where Are We 205 – The Atacama Large 309 – Galaxies and AGN II Now and Where Are We Going? Millimeter/submillimeter Array: A New 310 – Young Stellar Objects, Star Formation 109 – Bridging Laboratory and Astrophysics: Window on the Universe and Star Clusters Molecules 208 – Galaxies and AGN I 311 – Curiosity on Mars: The Latest Results 110 – Interstellar Medium, Dust, Etc. 209 – Supernovae and Neutron -
Stars and Galaxies
Stars and Galaxies STUDENT PAGE Se e i n g i n to t h e Pa S t A galaxy is a gravitationally bound system of stars, gas, and dust. Gal- We can’t travel into the past, but we axies range in diameter from a few thousand to a few hundred thou- can get a glimpse of it. Every sand light-years. Each galaxy contains billions (10 9) or trillions (1012) time we look at the Moon, for of stars. In this activity, you will apply concepts of scale to grasp the example, we see it as it was a distances between stars and galaxies. You will use this understanding little more than a second ago. to elaborate on the question, Do galaxies collide? That’s because sunlight reflected from the Moon’s surface takes a little more EX P LORE than a second to reach Earth. We see On a clear, dark night, you can see hundreds of bright stars. The next table the Sun as it looked about eight minutes shows some of the brightest stars with their diameters and distances from ago, and the other stars as they were a the Sun. Use a calculator to determine the scaled distance to each star few years to a few centuries ago. (how many times you could fit the star between itself and the Sun). Hint: And then there’s M31, the Androm- you first need to convert light-years and solar diameters into meters. One eda galaxy — the most distant object light-year equals 9.46 x 1015 meters, and the Sun’s diameter is 1.4 x 109 that’s readily visible to human eyes. -
Extragalactic Astronomy: the U Nivcre Bey Nd Our Galaxy
U1IJT RESUPE EU 1J3 199 021 775 dacon Eenneth Char TITLE Extragalactic Astronomy: The U nivcre Bey nd Our Galaxy. American Astronomical Society, Princeton, N.J. SFONS AGENCY National Aeronautics and Space Administra ashingtonl D.C.; National Science Foundation, Washington, D.C. REPOBT NO NASA-i:T-129 PUB DATE Sep 76 NOTE 44p.; FOF ltEd aocunents, _e SE 021 773-776 AVAII,AULE Superintendent of Documents, U.S. G-vernment Prin ing Office, Washington, D.C. 20402(5 ock Number 033-000-00657-8, $1.30) E.-RS PE10E 1F-$0.03 HC-$2.06 Plus Postige. DESCilIPTORS *Astronomy; Curriculum; *Instructional Materials; Science Education; *Scientific iesearch; Secondary Education; *Secondary School Science; *Space Sciences TIF NASA; National Aeronautics and Space Administration BSTRACT This booklet is part of an American Astronomical Society curriculum project designed to provide teaching materials to teachers or secondary school chemistry, physics, and earth science. The material is presented in three parts: one section provides the fundamental content of extragalactic astronomy, another section discusses modern discoveries in detail, and the last section summarizes the earlier discussions within the structure of the Big Bang Theory of Evolution. Each of the three sections is followed by student exercises and activities, laboratory projects, and questions and answers. The glossary contains unfamiliar terms used in the text and a collection of teacher aids such as literature references and audiovisual materials. (111) ***** *** * ** ** ***************** ********** Document., acquired by IC include many informal unpublished aterials not available from other sources. ERIC makes every effort * * to obtain the best copy available. Nevertheless, items of marginal * * reproducibility are often encountered and tbis affects the quality * * of the microfiche and hardcopy reproductions ERIC makes available * * via the ERIC Document Reproduction Service (EDRS).