Chapter 1 Our Place in the Universe
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Constructing a Galactic Coordinate System Based on Near-Infrared and Radio Catalogs
A&A 536, A102 (2011) Astronomy DOI: 10.1051/0004-6361/201116947 & c ESO 2011 Astrophysics Constructing a Galactic coordinate system based on near-infrared and radio catalogs J.-C. Liu1,2,Z.Zhu1,2, and B. Hu3,4 1 Department of astronomy, Nanjing University, Nanjing 210093, PR China e-mail: [jcliu;zhuzi]@nju.edu.cn 2 key Laboratory of Modern Astronomy and Astrophysics (Nanjing University), Ministry of Education, Nanjing 210093, PR China 3 Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210008, PR China 4 Graduate School of Chinese Academy of Sciences, Beijing 100049, PR China e-mail: [email protected] Received 24 March 2011 / Accepted 13 October 2011 ABSTRACT Context. The definition of the Galactic coordinate system was announced by the IAU Sub-Commission 33b on behalf of the IAU in 1958. An unrigorous transformation was adopted by the Hipparcos group to transform the Galactic coordinate system from the FK4-based B1950.0 system to the FK5-based J2000.0 system or to the International Celestial Reference System (ICRS). For more than 50 years, the definition of the Galactic coordinate system has remained unchanged from this IAU1958 version. On the basis of deep and all-sky catalogs, the position of the Galactic plane can be revised and updated definitions of the Galactic coordinate systems can be proposed. Aims. We re-determine the position of the Galactic plane based on modern large catalogs, such as the Two-Micron All-Sky Survey (2MASS) and the SPECFIND v2.0. This paper also aims to propose a possible definition of the optimal Galactic coordinate system by adopting the ICRS position of the Sgr A* at the Galactic center. -
Star Planet Moon (Or Satellite)
1/17/12 " Chapter 1" 1) WhatStar is this? Our Place in the Universe A large, glowing ball of gas that generates heat and light through nuclear fusion 2) WhatPlanet is this? Moon3)What (or issatellite) this? An object that orbits a planet. Mars Neptune A moderately large object that orbits a star; it shines by reflected light. May be rocky, icy, or Ganymede (orbits Jupiter) gaseous in composition. 1 1/17/12 4) AsteroidWhat is this? 5) WhatComet is this? A relatively A relatively small small and icy and rocky object object that orbits a star. that orbits a star. Ida 6)WhatStar System is this? 7) WhatNebula is this? A star and all the material that orbits it, including its planets and moons An interstellar cloud of gas and/or dust 2 1/17/12 8) WhatGalaxy is this? A great island of stars in space, all held 9) UniverseWhat is this? together by gravity and orbiting a common center The sum total of all matter and energy; that is, everything within and between all galaxies M31, The Great Galaxy in Andromeda What is our place in the universe? How did we come to be? 3 1/17/12 How can we know what the universe was like in the past? Example: • Light travels at a finite speed (300,000 km/s). We see the Orion Nebula as it Destination Light travel time looked 1,500 Moon 1 second years ago. Sun 8 minutes Nearest Star 4 years Andromeda Galaxy 2.5 million years • Thus, we see objects as they were in the past: The farther away we look in distance, ! the further back we look in time. -
Elements of Astronomy and Cosmology Outline 1
ELEMENTS OF ASTRONOMY AND COSMOLOGY OUTLINE 1. The Solar System The Four Inner Planets The Asteroid Belt The Giant Planets The Kuiper Belt 2. The Milky Way Galaxy Neighborhood of the Solar System Exoplanets Star Terminology 3. The Early Universe Twentieth Century Progress Recent Progress 4. Observation Telescopes Ground-Based Telescopes Space-Based Telescopes Exploration of Space 1 – The Solar System The Solar System - 4.6 billion years old - Planet formation lasted 100s millions years - Four rocky planets (Mercury Venus, Earth and Mars) - Four gas giants (Jupiter, Saturn, Uranus and Neptune) Figure 2-2: Schematics of the Solar System The Solar System - Asteroid belt (meteorites) - Kuiper belt (comets) Figure 2-3: Circular orbits of the planets in the solar system The Sun - Contains mostly hydrogen and helium plasma - Sustained nuclear fusion - Temperatures ~ 15 million K - Elements up to Fe form - Is some 5 billion years old - Will last another 5 billion years Figure 2-4: Photo of the sun showing highly textured plasma, dark sunspots, bright active regions, coronal mass ejections at the surface and the sun’s atmosphere. The Sun - Dynamo effect - Magnetic storms - 11-year cycle - Solar wind (energetic protons) Figure 2-5: Close up of dark spots on the sun surface Probe Sent to Observe the Sun - Distance Sun-Earth = 1 AU - 1 AU = 150 million km - Light from the Sun takes 8 minutes to reach Earth - The solar wind takes 4 days to reach Earth Figure 5-11: Space probe used to monitor the sun Venus - Brightest planet at night - 0.7 AU from the -
The Milky Way Almost Every Star We Can See in the Night Sky Belongs to Our Galaxy, the Milky Way
The Milky Way Almost every star we can see in the night sky belongs to our galaxy, the Milky Way. The Galaxy acquired this unusual name from the Romans who referred to the hazy band that stretches across the sky as the via lactia, or “milky road”. This name has stuck across many languages, such as French (voie lactee) and spanish (via lactea). Note that we use a capital G for Galaxy if we are talking about the Milky Way The Structure of the Milky Way The Milky Way appears as a light fuzzy band across the night sky, but we also see individual stars scattered in all directions. This gives us a clue to the shape of the galaxy. The Milky Way is a typical spiral or disk galaxy. It consists of a flattened disk, a central bulge and a diffuse halo. The disk consists of spiral arms in which most of the stars are located. Our sun is located in one of the spiral arms approximately two-thirds from the centre of the galaxy (8kpc). There are also globular clusters distributed around the Galaxy. In addition to the stars, the spiral arms contain dust, so that certain directions that we looked are blocked due to high interstellar extinction. This dust means we can only see about 1kpc in the visible. Components in the Milky Way The disk: contains most of the stars (in open clusters and associations) and is formed into spiral arms. The stars in the disk are mostly young. Whilst the majority of these stars are a few solar masses, the hot, young O and B type stars contribute most of the light. -
Arxiv:1307.0569V1
IAUS 298 Setting the scence for Gaia and LAMOST Proceedings IAU Symposium No. 298, 2014 c 2014 International Astronomical Union S. Feltzing, G. Zhao, N. A. Walton & P. A. Whitelock, eds. DOI: 00.0000/X000000000000000X The Milky Way thin disk structure as revealed by stars and young open clusters Giovanni Carraro Alonso de Cordova 3107, 19001, Santiago de Chile, Chile email: [email protected] Abstract. In this contribution I shall focus on the structure of the Galactic thin disk. The evolution of the thin disk and its chemical properties have been discussed in detail by T. Bensby’s contribution in conjunction with the properties of the Galactic thick disk, and by L.Olivia in conjunction with the properties of the Galactic bulge. I will review and discuss the status of our understanding of three major topics, which have been the subject of intense research nowadays, after long years of silence: (1) the spiral structure of the Milky Way, (2) the size of the Galactic disk, and (3) the nature of the Local arm (Orion spur), where the Sun is immersed. The provisional conclusions of this discussion are that : (1) we still have quite a poor knowledge of the Milky Way spiral structure, and the main dis-agreements among various tracers are still to be settled; (2) the Galactic disk does clearly not have an obvious luminous cut-off at about 14 kpc from the Galactic center, and next generation Galactic models need to be updated in this respect, and (3) the Local arm is most probably an inter-arm structure, similar to what we see in several external spirals, like M 74. -
Orbits of Massive Satellite Galaxies: I. a Close Look at the Large Magellanic Cloud and a New Orbital History for M33
MNRAS 000,1{28 (2016) Preprint 17 November 2016 Compiled using MNRAS LATEX style file v3.0 Orbits of Massive Satellite Galaxies: I. A Close Look at the Large Magellanic Cloud and a New Orbital History for M33 Ekta Patel,1? Gurtina Besla,1 and Sangmo Tony Sohn2 1Department of Astronomy, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USA 2Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA Accepted XXX. Received YYY; in original form ZZZ ABSTRACT The Milky Way (MW) and M31 both harbor massive satellite galaxies, the Large Mag- ellanic Cloud (LMC) and M33, which may comprise up to 10 per cent of their host's total mass. Massive satellites can change the orbital barycentre of the host-satellite system by tens of kiloparsecs and are cosmologically expected to harbor dwarf satellite galaxies of their own. Assessing the impact of these effects depends crucially on the orbital histories of the LMC and M33. Here, we revisit the dynamics of the MW-LMC system and present the first detailed analysis of the M31-M33 system utilizing high precision proper motions and statistics from the dark matter-only Illustris cosmolog- ical simulation. With the latest Hubble Space Telescope proper motion measurements of M31, we reliably constrain M33's interaction history with its host. In particular, like the LMC, M33 is either on its first passage (tinf < 2 Gyr ago) or if M31 is massive 12 (≥ 2 × 10 M ), it is on a long period orbit of about 6 Gyr. Cosmological analogs of the LMC and M33 identified in Illustris support this picture and provide further insight about their host masses. -
Milky Way Haze
CURIOSITY AT HOME MILKY WAY HAZE A galaxy is a group of stars, gas and dust. Our solar system is part of the Milky Way Galaxy. This galaxy appears as a milky haze in the night sky. Have you ever wondered why the Milky Way resembles a hazy, cloud-like strip in the sky? MATERIALS • Paper hole punch • Glue • Black construction paper • White paper • Masking or painter’s tape • Pen • Paper or science notebook PROCEDURE • Use the hole punch to cut out 50 circles from the white paper. • Glue the circles very close together in the center of the black sheet of paper. • Tape the black construction paper to a pole, tree, wall or other outside object you will be able to see from a distance. • Stand so your nose is almost touching the black construction paper. • Draw or write about your observations on a piece of paper or in your science notebook. • Slowly back away until the separate circles can no longer be seen. • Estimate or measure how far away you were when you could no longer see the separate circles. • What do you notice about the circles seen from a distance as compared to close up? DID YOU KNOW Our eyes are unable to distinguish small points of light that are very close together. Rather, the separate points of light blend together. In our galaxy, the light from distant stars blends together to form the Milky Way haze. The Milky Way galaxy is home to all of the stars that are visible to the naked eye as well as billions of stars that are so far away our eyes are unable to distinguish each individual point of star light. -
Size and Scale Attendance Quiz II
Size and Scale Attendance Quiz II Are you here today? Here! (a) yes (b) no (c) are we still here? Today’s Topics • “How do we know?” exercise • Size and Scale • What is the Universe made of? • How big are these things? • How do they compare to each other? • How can we organize objects to make sense of them? What is the Universe made of? Stars • Stars make up the vast majority of the visible mass of the Universe • A star is a large, glowing ball of gas that generates heat and light through nuclear fusion • Our Sun is a star Planets • According to the IAU, a planet is an object that 1. orbits a star 2. has sufficient self-gravity to make it round 3. has a mass below the minimum mass to trigger nuclear fusion 4. has cleared the neighborhood around its orbit • A dwarf planet (such as Pluto) fulfills all these definitions except 4 • Planets shine by reflected light • Planets may be rocky, icy, or gaseous in composition. Moons, Asteroids, and Comets • Moons (or satellites) are objects that orbit a planet • An asteroid is a relatively small and rocky object that orbits a star • A comet is a relatively small and icy object that orbits a star Solar (Star) System • A solar (star) system consists of a star and all the material that orbits it, including its planets and their moons Star Clusters • Most stars are found in clusters; there are two main types • Open clusters consist of a few thousand stars and are young (1-10 million years old) • Globular clusters are denser collections of 10s-100s of thousand stars, and are older (10-14 billion years -
NGC 602: Taken Under the “Wing” of the Small Magellanic Cloud
National Aeronautics and Space Administration NGC 602 www.nasa.gov NGC 602: Taken Under the “Wing” of the Small Magellanic Cloud The Small Magellanic Cloud (SMC) is one of the closest galaxies to the Milky Way. In this composite image the Chandra data is shown in purple, optical data from Hubble is shown in red, green and blue and infrared data from Spitzer is shown in red. Chandra observations of the SMC have resulted in the first detection of X-ray emission from young stars with masses similar to our Sun outside our Milky Way galaxy. The Small Magellanic Cloud (SMC) is one of the Milky Way’s region known as NGC 602, which contains a collection of at least closest galactic neighbors. Even though it is a small, or so-called three star clusters. One of them, NGC 602a, is similar in age, dwarf galaxy, the SMC is so bright that it is visible to the unaided mass, and size to the famous Orion Nebula Cluster. Researchers eye from the Southern Hemisphere and near the equator. have studied NGC 602a to see if young stars—that is, those only a few million years old—have different properties when they have Modern astronomers are also interested in studying the SMC low levels of metals, like the ones found in NGC 602a. (and its cousin, the Large Magellanic Cloud), but for very different reasons. The SMC is one of the Milky Way’s closest galactic Using Chandra, astronomers discovered extended X-ray emission, neighbors. Because the SMC is so close and bright, it offers an from the two most densely populated regions in NGC 602a. -
Cosmic Dragon Breathes New Life Into the Night
SPACE SCOOP NEWS DA TUTTO L’UNIVERSO 27Cosmic Novembre Dragon 2013 Breathes New Life into the Night Sky The distances between stars are so immense that we can't use miles or kilometres to measure them, the numbers would become too large. For example, the closest star to our Solar System, is a whopping 38,000,000,000,000 kilometres away! And that's the closest star. There are stars that are billions of times farther away than that. No one wants to write or talk about numbers that have 20 digits in them! So, for distances in space we use a different measurement: the time taken for a light beam to travel. When travelling through space, light moves at a set speed of nearly 300,000 kilometres per second. Nothing in the known universe travels faster than the speed of light. If you somehow managed to cheat the laws of physics and travel as fast as a ray of light, it would still take 160 000 years to reach the object in this photograph! And this cloud is inside one of the Milky Way’s closest neighbours, a nearby galaxy called the Large Magellanic Cloud. This new image explores colourful clouds of gas and dust called NGC 2035 (seen on the right), sometimes nicknamed the Dragon’s Head Nebula. The colourful clouds of gas and dust are filled with hot new-born stars which make these clouds glow. They're also regions where stars have ended their lives in terrific blazes of glory as supernova explosions. Looking at this image, it may be difficult to grasp the sheer size of these clouds — we call the distance light can travel in a year a “light-year” and -
Large Magellanic Cloud, One of Our Busy Galactic Neighbors
The Large Magellanic Cloud, One of Our Busy Galactic Neighbors www.nasa.gov Our Busy Galactic Neighbors also contain fewer metals or elements heavier than hydrogen and helium. Such an environment is thought to slow the growth The cold dust that builds blazing stars is revealed in this image of stars. Star formation in the universe peaked around 10 billion that combines infrared observations from the European Space years ago, even though galaxies contained lesser abundances Agency’s Herschel Space Observatory and NASA’s Spitzer of metallic dust. Previously, astronomers only had a general Space Telescope. The image maps the dust in the galaxy known sense of the rate of star formation in the Magellanic Clouds, as the Large Magellanic Cloud, which, with the Small Magellanic but the new images enable them to study the process in more Cloud, are the two closest sizable neighbors to our own Milky detail. Way Galaxy. Herschel is a European The Large Magellanic Cloud looks like a fiery, circular explosion Space Agency in the combined Herschel–Spitzer infrared data. Ribbons of dust cornerstone mission, ripple through the galaxy, with significant fields of star formation with science instruments noticeable in the center, center-left and top right. The brightest provided by consortia center-left region is called 30 Doradus, or the Tarantula Nebula, of European institutes for its appearance in visible light. and with important participation by NASA. NASA’s Herschel Project Office is based at NASA’s Jet Propulsion Laboratory, Pasadena, Calif. JPL contributed mission-enabling technology for two of Herschel’s three science instruments. -
Search for Blue Compact Dwarf Galaxies During Quiescence
The Astrophysical Journal, 685:194Y210, 2008 September 20 A # 2008. The American Astronomical Society. All rights reserved. Printed in U.S.A. SEARCH FOR BLUE COMPACT DWARF GALAXIES DURING QUIESCENCE J. Sa´nchez Almeida,1 C. Mun˜oz-Tun˜o´n,1 R. Amor´ıIn,1 J. A. Aguerri,1 R. Sa´nchez-Janssen,1 and G. Tenorio-Tagle2 Received 2008 February 7; accepted 2008 May 21 ABSTRACT Blue compact dwarf (BCD) galaxies are metal-poor systems going through a major starburst that cannot last for long. We have identified galaxies which may be BCDs during quiescence (QBCD), i.e., before the characteristic starburst sets in or when it has faded away. These QBCD galaxies are assumed to be like the BCD host galaxies. The SDSS DR6 database provides 21,500 QBCD candidates. We also select from SDSS DR6 a complete sample of BCD galaxies to serve as reference. The properties of these two galaxy sets have been computed and compared. The QBCD candidates are 30 times more abundant than the BCDs, with their luminosity functions being very similar except for the scaling factor and the expected luminosity dimming associated with the end of the starburst. QBCDs are redder than BCDs, and they have larger H ii regionYbased oxygen abundance. QBCDs also have lower surface bright- ness. The BCD candidates turn out to be the QBCD candidates with the largest specific star formation rate (actually, with the largest H equivalent width). One out of every three dwarf galaxies in the local universe may be a QBCD. The properties of the selected BCDs and QBCDs are consistent with a single sequence in galactic evolution, which the quiescent phase lasting 30 times longer than the starburst phase.