Core of Omega Centauri (NGC 5139) Lithograph As the Initial Source of These Are Terms Students May Encounter While Doing Further Research on Stellar Evolution
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Arxiv:1910.11169V1 [Astro-Ph.EP] 24 Oct 2019 Metchev Et Al.(2004) Due to the Detection of a Strong Mid- Tinuum and at HCO+ and CO Gas Emission Lines
Astronomy & Astrophysics manuscript no. PDS70_v2 c ESO 2019 October 25, 2019 VLT/SPHERE exploration of the young multiplanetary system PDS70? D. Mesa1, M. Keppler2, F. Cantalloube2, L. Rodet3, B. Charnay4, R. Gratton1, M. Langlois5; 6, A. Boccaletti4, M. Bonnefoy3, A. Vigan6, O. Flasseur7, J. Bae8, M. Benisty3; 9, G. Chauvin3; 9, J. de Boer10, S. Desidera1, T. Henning2, A.-M. Lagrange3, M. Meyer11, J. Milli12, A. Müller2, B. Pairet13, A. Zurlo14; 15; 6, S. Antoniucci16, J.-L. Baudino17, S. Brown Sevilla2, E. Cascone18, A. Cheetham19, R.U. Claudi1, P. Delorme3, V. D’Orazi1, M. Feldt2, J. Hagelberg19, M. Janson20, Q. Kral4, E. Lagadec21, C. Lazzoni1, R. Ligi22, A.-L. Maire2; 23, P. Martinez21, F. Menard3, N. Meunier3, C. Perrot4; 24; 25, S. Petrus3, C. Pinte26; 3, E.L. Rickman19, S. Rochat3, D. Rouan4, M. Samland2; 20, J.-F. Sauvage27; 6, T. Schmidt4; 28, S. Udry19, L. Weber19, F. Wildi19 (Affiliations can be found after the references) Received / accepted ABSTRACT Context. PDS 70 is a young (5.4 Myr), nearby (∼113 pc) star hosting a known transition disk with a large gap. Recent observations with SPHERE and NACO in the near-infrared (NIR) allowed us to detect a planetary mass companion, PDS 70 b, within the disk cavity. Moreover, observations in Hα with MagAO and MUSE revealed emission associated to PDS 70 b and to another new companion candidate, PDS 70 c, at a larger separation from the star. PDS 70 is the only multiple planetary system at its formation stage detected so far through direct imaging. Aims. Our aim is to confirm the discovery of the second planet PDS 70 c using SPHERE at VLT, to further characterize its physical properties, and search for additional point sources in this young planetary system. -
Issue 59, Yir 2015
1 Director’s Message 50 Fast Turnaround Program Markus Kissler-Patig Pilot Underway Rachel Mason 3 Probing Time Delays in a Gravitationally Lensed Quasar 54 Base Facility Operations Keren Sharon Gustavo Arriagada 7 GPI Discovers the Most Jupiter-like 58 GRACES: The Beginning of a Exoplanet Ever Directly Detected Scientific Legacy Julien Rameau and Robert De Rosa André-Nicolas Chené 12 First Likely Planets in a Nearby 62 The New Cloud-based Gemini Circumbinary Disk Observatory Archive Valerie Rapson Paul Hirst 16 RCW 41: Dissecting a Very Young 65 Solar Panel System Installed at Cluster with Adaptive Optics Gemini North Benoit Neichel Alexis-Ann Acohido 21 Science Highlights 67 Gemini Legacy Image Releases Nancy A. Levenson Gemini staff contributions 30 On the Horizon 72 Journey Through the Universe Gemini staff contributions Janice Harvey 37 News for Users 75 Viaje al Universo Gemini staff contributions Maria-Antonieta García 46 Adaptive Optics at Gemini South Gaetano Sivo, Vincent Garrel, Rodrigo Carrasco, Markus Hartung, Eduardo Marin, Vanessa Montes, and Chad Trujillo ON THE COVER: GeminiFocus January 2016 A montage featuring GeminiFocus is a quarterly publication a recent Flamingos-2 of the Gemini Observatory image of the galaxy 670 N. A‘ohoku Place, Hilo, Hawai‘i 96720, USA NGC 253’s inner region Phone: (808) 974-2500 Fax: (808) 974-2589 (as discussed in the Science Highlights Online viewing address: section, page 21; with www.gemini.edu/geminifocus an inset showing the Managing Editor: Peter Michaud stellar supercluster Science Editor: Nancy A. Levenson identified as the galaxy’s nucleus) Associate Editor: Stephen James O’Meara and cover pages Designer: Eve Furchgott/Blue Heron Multimedia from each of issue of Any opinions, findings, and conclusions or GeminiFocus in 2015. -
The Nearest Stars: a Guided Tour by Sherwood Harrington, Astronomical Society of the Pacific
www.astrosociety.org/uitc No. 5 - Spring 1986 © 1986, Astronomical Society of the Pacific, 390 Ashton Avenue, San Francisco, CA 94112. The Nearest Stars: A Guided Tour by Sherwood Harrington, Astronomical Society of the Pacific A tour through our stellar neighborhood As evening twilight fades during April and early May, a brilliant, blue-white star can be seen low in the sky toward the southwest. That star is called Sirius, and it is the brightest star in Earth's nighttime sky. Sirius looks so bright in part because it is a relatively powerful light producer; if our Sun were suddenly replaced by Sirius, our daylight on Earth would be more than 20 times as bright as it is now! But the other reason Sirius is so brilliant in our nighttime sky is that it is so close; Sirius is the nearest neighbor star to the Sun that can be seen with the unaided eye from the Northern Hemisphere. "Close'' in the interstellar realm, though, is a very relative term. If you were to model the Sun as a basketball, then our planet Earth would be about the size of an apple seed 30 yards away from it — and even the nearest other star (alpha Centauri, visible from the Southern Hemisphere) would be 6,000 miles away. Distances among the stars are so large that it is helpful to express them using the light-year — the distance light travels in one year — as a measuring unit. In this way of expressing distances, alpha Centauri is about four light-years away, and Sirius is about eight and a half light- years distant. -
Star Clusters
Star Clusters • Eventually, photons and stellar winds clear out the remaining gas and dust and leave behind the stars. • Reflection nebulae provide evidence for remaining dust on the far side of the Pleiades Star Clusters • It may be that all stars are born in clusters. • A good question is therefore why are most stars we see in the Galaxy not members of obvious clusters? • The answer is that the majority of newly-formed clusters are very weakly gravitationally bound. Perturbations from passing molecular clouds, spiral arms or mass loss from the cluster stars `unbind’ most clusters. Star Cluster Ages • We can use the H-R Diagram of the stars in a cluster to determine the age of the cluster. • A cluster starts off with stars along the full main sequence. • Because stars with larger mass evolve more quickly, the hot, luminous end of the main sequence becomes depleted with time. • The `main-sequence turnoff’ moves to progressively lower mass, L and T with time. • Young clusters contain short-lived, massive stars in their main sequence • Other clusters are missing the high-mass MSTO stars and we can infer the cluster age is the main-sequence lifetime of the highest mass star still on the main- sequence. 25Mo 3million years 104 3Mo 500Myrs 102 1M 10Gyr L o 1 0.5Mo 200Gyr 10-2 30000 15000 7500 3750 Temperature Star Clusters Sidetrip • There are two basic types of clusters in the Galaxy. • Globular Clusters are mostly in the halo of the Galaxy, contain >100,000 stars and are very ancient. • Open clusters are in the disk, contain between several and a few thousand stars and range in age from 0 to 10Gyr Galaxy Ages • Deriving galaxy ages is much harder because most galaxies have a star formation history rather than a single-age population of stars. -
The Radio Continuum View of Centaurus Acentaurus A
TheThe radioradio continuumcontinuum viewview ofof CentaurusCentaurus AA Ron Ekers CSIRO The Many Faces of Centaurus A Sydney, 29 June 2009 Ilana's composite Morganti et al. 1999 9° 10' Burns et al. xx image courtesy Norbert Junkes (MPIfR) WhyWhy CentaurusCentaurus AA isis specialspecial ■ the first extragalactic radio source ■ the brightest source in the Southern Hemisphere ■ the second double lobed source discovered ± after Cygnus A ■ the closest Radio Galaxy ■ the closest AGN ■ the closest SMBH ± VLBI resolution 0.01pc, 100 Rs ■ A spectacular galaxy EvolutionEvolution ofof thethe ModelsModels ■ Radio sources ± Static magnetic field 1960 ± Evolutionary sequence 1970 ± Continuous injection ± Continuous reacceleration ■ Energy source ± Galaxy collisions 1950's ± Nuclear accretions 1960- ± Accretion triggered by collisions 1980- CentaurusCentaurus AA thethe closestclosest AGNAGN ■ Distance 3.4Mpc ■ Next closest comparable AGN M87 17Mpc ! ■ Average distance to a L=1024 W Hz-1 radio galaxies ± 10Mpc ± So we are lucky (or influenced!) ■ Much easier to study at all wavelengths ■ Subtends a large angular size ± Good linear resolution ± Background probes SomeSome RadioRadio GalaxiesGalaxies Name Size Log Log (kpc) Luminosity Energy (ergs sec-1) (ergs) Centaurus A 470 41.7 59.9 Cygnus A 200 45.2 60.6 M87 80 42.0 58.6 M82 1 39.5 55.2 PolarizationPolarization inin CentaurusCentaurus AA Bracewell 1962 ■ April 1962 ■ Parkes 64m just completed ■ Discovered by Bracewell ± Published Cooper and Price ± Visitors Log ± Not a National Facilities yet! ■ Connie -
TESS Discovery of a Super-Earth and Three Sub-Neptunes Hosted by the Bright, Sun-Like Star HD 108236
Swarthmore College Works Physics & Astronomy Faculty Works Physics & Astronomy 2-1-2021 TESS Discovery Of A Super-Earth And Three Sub-Neptunes Hosted By The Bright, Sun-Like Star HD 108236 T. Daylan K. Pinglé J. Wright M. N. Günther K. G. Stassun Follow this and additional works at: https://works.swarthmore.edu/fac-physics See P nextart of page the forAstr additionalophysics andauthors Astr onomy Commons Let us know how access to these works benefits ouy Recommended Citation T. Daylan, K. Pinglé, J. Wright, M. N. Günther, K. G. Stassun, S. R. Kane, A. Vanderburg, D. Jontof-Hutter, J. E. Rodriguez, A. Shporer, C. X. Huang, T. Mikal-Evans, M. Badenas-Agusti, K. A. Collins, B. V. Rackham, S. N. Quinn, R. Cloutier, K. I. Collins, P. Guerra, Eric L.N. Jensen, J. F. Kielkopf, B. Massey, R. P. Schwarz, D. Charbonneau, J. J. Lissauer, J. M. Irwin, Ö Baştürk, B. Fulton, A. Soubkiou, B. Zouhair, S. B. Howell, C. Ziegler, C. Briceño, N. Law, A. W. Mann, N. Scott, E. Furlan, D. R. Ciardi, R. Matson, C. Hellier, D. R. Anderson, R. P. Butler, J. D. Crane, J. K. Teske, S. A. Shectman, M. H. Kristiansen, I. A. Terentev, H. M. Schwengeler, G. R. Ricker, R. Vanderspek, S. Seager, J. N. Winn, J. M. Jenkins, Z. K. Berta-Thompson, L. G. Bouma, W. Fong, G. Furesz, C. E. Henze, E. H. Morgan, E. Quintana, E. B. Ting, and J. D. Twicken. (2021). "TESS Discovery Of A Super-Earth And Three Sub-Neptunes Hosted By The Bright, Sun-Like Star HD 108236". -
Andrea Possenti
UniversidadUniversidad dede ValenciaValencia 1515November November2010 2010 PulsarsPulsars asas probesprobes forfor thethe existenceexistence ofof IMBHsIMBHs ANDREA POSSENTI LayoutLayout ¾¾ KnownKnown BlackBlack HoleHole classesclasses ¾¾ FormationFormation scenariosscenarios forfor thethe IMBHsIMBHs ¾¾ IMBHIMBH candidatescandidates ¾¾ IMBHIMBH candidatescandidates (?)(?) fromfrom RadioRadio PulsarPulsar datadata analysisanalysis ¾¾ PerspectivesPerspectives forfor thethe directdirect observationobservation ofof IMBHsIMBHs fromfrom PulsarPulsar searchessearches ClassesClasses ofof BlackBlack HolesHoles Stellar mass Black Holes resulting from star evolution are supposed to be contained in many X-ray binaries: for solar metallicity, the max mass is of order few 10 Msun Massive Black Holes seen in the nucleus of the galaxies: 6 9 masses of order ≈ 10 Msun to ≈ 10 Msun AreAre IntermediateIntermediate Mass Black Holes ((IMBH)IMBH) ofof massesmasses ≈≈ 100100 -- 10,000 10,000 MMsunsun alsoalso partpart ofof thethe astronomicalastronomical landscapelandscape ?? N.B. ULX in the Globular Cluster RZ2109 of NGC 4472 may be a stellar mass BH likely in a triple system [ Maccarone et al. 2007 - 2010 ] FormationFormation mechanismsmechanisms forfor IMBHsIMBHs 11- - Mass Mass segregationsegregation ofof compactcompact remnantsremnants inin aa densedense starstar cluster 22– – Runaway Runaway collisionscollisions ofof massivemassive starsstars inin aa densedense starstar clustercluster In both cases, the seed IMBH can then grow by capturing other “ordinary” -
Gli Ammassi Di Galassie
Universo in Fiore 2017 CORSO BASE I GIGANTI DEL COSMO: GLI AMMASSI DI GALASSIE Sabrina De Grandi [email protected] Organizzazione spaziale delle galassie Ammassi Gruppi Galassie 100 mila a.l. ~30 kpc 3 milioni a.l. ~ 103 kpc 20 milioni a.l. ~ 7x103 kpc I primi cataloghi di ammassi Fino agli anni ’80: ispezione visuale di lastre fotografiche alla ricerca di sovradensita` di galassie. Es. di lastre fotografiche: • PSS: National Geographic Society-Palomar Observatory Sky Survey (Telescopio 5m Hale, Mt. Wilson US) • UKST: Schmidt telescope IIIa-J plates (Telescopio 1.2m, UK-Australia),… I cataloghi di Abell (1958) e Zwicky (1961-1968) Il catalogo piu` usato: Abell (1958) Emisfero Nord (2712) e A.C.O. (1989) Emisfero Sud (1364). 1958: Abell ispeziono` di 104 deg2 di lastre PSS (Luna ~0.25 deg2) Criteri principali: • almeno 30 galassie • compatto (0.02<z<0.2) • piano galattico escluso Dagli anni ’90: • algoritmi automatici di identificazione al posto dell’occhio umano. • Non più lastre fotografiche, ma immagini digitali (CCD) • SDSS (Sloan Digital Sky Survey), iniziata nel 2000 e tutt’ora in atto (35% del cielo osservato, 500 milioni di oggetti, catalogo di ammassi • Accesso libero ai dati (nel Telescopio dedicato ad 2015: 13o Data Release) Apache Point 2.5m (US) Immagine SDSS dell’ammasso A2142 MACS J1206.2-0847 DIAMETRO tipico di un ammasso di galassie ~ 20 milioni anni luce ~ 7 Mpc SPICA (훼 costellazione della Vergine) MACS J1206.2-0847 DIAMETRO tipico di un ammasso di galassie ~ 20 milioni anni luce ~ 7 Mpc ma… DISTANZA di MACS J1206 ~ 4.5 miliardi di anni luce ~ 1500 Mpc Dove si trova la Via Lattea in questa struttura universale? ovvero Noi ci troviamo in un Ammasso di galassie? Il Gruppo Locale 100.000 a.l. -
Stellar Distances Teacher Guide
Stars and Planets 1 TEACHER GUIDE Stellar Distances Our Star, the Sun In this Exploration, find out: ! How do the distances of stars compare to our scale model solar system?. ! What is a light year? ! How long would it take to reach the nearest star to our solar system? (Image Credit: NASA/Transition Region & Coronal Explorer) Note: The above image of the Sun is an X -ray view rather than a visible light image. Stellar Distances Teacher Guide In this exercise students will plan a scale model to explore the distances between stars, focusing on Alpha Centauri, the system of stars nearest to the Sun. This activity builds upon the activity Sizes of Stars, which should be done first, and upon the Scale in the Solar System activity, which is strongly recommended as a prerequisite. Stellar Distances is a math activity as well as a science activity. Necessary Prerequisite: Sizes of Stars activity Recommended Prerequisite: Scale Model Solar System activity Grade Level: 6-8 Curriculum Standards: The Stellar Distances lesson is matched to: ! National Science and Math Education Content Standards for grades 5-8. ! National Math Standards 5-8 ! Texas Essential Knowledge and Skills (grades 6 and 8) ! Content Standards for California Public Schools (grade 8) Time Frame: The activity should take approximately 45 minutes to 1 hour to complete, including short introductions and follow-ups. Purpose: To aid students in understanding the distances between stars, how those distances compare with the sizes of stars, and the distances between objects in our own solar system. © 2007 Dr Mary Urquhart, University of Texas at Dallas Stars and Planets 2 TEACHER GUIDE Stellar Distances Key Concepts: o Distances between stars are immense compared with the sizes of stars. -
Stsci Newsletter: 2011 Volume 028 Issue 02
National Aeronautics and Space Administration Interacting Galaxies UGC 1810 and UGC 1813 Credit: NASA, ESA, and the Hubble Heritage Team (STScI/AURA) 2011 VOL 28 ISSUE 02 NEWSLETTER Space Telescope Science Institute We received a total of 1,007 proposals, after accounting for duplications Hubble Cycle 19 and withdrawals. Review process Proposal Selection Members of the international astronomical community review Hubble propos- als. Grouped in panels organized by science category, each panel has one or more “mirror” panels to enable transfer of proposals in order to avoid conflicts. In Cycle 19, the panels were divided into the categories of Planets, Stars, Stellar Rachel Somerville, [email protected], Claus Leitherer, [email protected], & Brett Populations and Interstellar Medium (ISM), Galaxies, Active Galactic Nuclei and Blacker, [email protected] the Inter-Galactic Medium (AGN/IGM), and Cosmology, for a total of 14 panels. One of these panels reviewed Regular Guest Observer, Archival, Theory, and Chronology SNAP proposals. The panel chairs also serve as members of the Time Allocation Committee hen the Cycle 19 Call for Proposals was released in December 2010, (TAC), which reviews Large and Archival Legacy proposals. In addition, there Hubble had already seen a full cycle of operation with the newly are three at-large TAC members, whose broad expertise allows them to review installed and repaired instruments calibrated and characterized. W proposals as needed, and to advise panels if the panelists feel they do not have The Advanced Camera for Surveys (ACS), Cosmic Origins Spectrograph (COS), the expertise to review a certain proposal. Fine Guidance Sensor (FGS), Space Telescope Imaging Spectrograph (STIS), and The process of selecting the panelists begins with the selection of the TAC Chair, Wide Field Camera 3 (WFC3) were all close to nominal operation and were avail- about six months prior to the proposal deadline. -
Planets and Exoplanets
NASE Publications Planets and exoplanets Planets and exoplanets Rosa M. Ros, Hans Deeg International Astronomical Union, Technical University of Catalonia (Spain), Instituto de Astrofísica de Canarias and University of La Laguna (Spain) Summary This workshop provides a series of activities to compare the many observed properties (such as size, distances, orbital speeds and escape velocities) of the planets in our Solar System. Each section provides context to various planetary data tables by providing demonstrations or calculations to contrast the properties of the planets, giving the students a concrete sense for what the data mean. At present, several methods are used to find exoplanets, more or less indirectly. It has been possible to detect nearly 4000 planets, and about 500 systems with multiple planets. Objetives - Understand what the numerical values in the Solar Sytem summary data table mean. - Understand the main characteristics of extrasolar planetary systems by comparing their properties to the orbital system of Jupiter and its Galilean satellites. The Solar System By creating scale models of the Solar System, the students will compare the different planetary parameters. To perform these activities, we will use the data in Table 1. Planets Diameter (km) Distance to Sun (km) Sun 1 392 000 Mercury 4 878 57.9 106 Venus 12 180 108.3 106 Earth 12 756 149.7 106 Marte 6 760 228.1 106 Jupiter 142 800 778.7 106 Saturn 120 000 1 430.1 106 Uranus 50 000 2 876.5 106 Neptune 49 000 4 506.6 106 Table 1: Data of the Solar System bodies In all cases, the main goal of the model is to make the data understandable. -
Atlas Menor Was Objects to Slowly Change Over Time
C h a r t Atlas Charts s O b by j Objects e c t Constellation s Objects by Number 64 Objects by Type 71 Objects by Name 76 Messier Objects 78 Caldwell Objects 81 Orion & Stars by Name 84 Lepus, circa , Brightest Stars 86 1720 , Closest Stars 87 Mythology 88 Bimonthly Sky Charts 92 Meteor Showers 105 Sun, Moon and Planets 106 Observing Considerations 113 Expanded Glossary 115 Th e 88 Constellations, plus 126 Chart Reference BACK PAGE Introduction he night sky was charted by western civilization a few thou - N 1,370 deep sky objects and 360 double stars (two stars—one sands years ago to bring order to the random splatter of stars, often orbits the other) plotted with observing information for T and in the hopes, as a piece of the puzzle, to help “understand” every object. the forces of nature. The stars and their constellations were imbued with N Inclusion of many “famous” celestial objects, even though the beliefs of those times, which have become mythology. they are beyond the reach of a 6 to 8-inch diameter telescope. The oldest known celestial atlas is in the book, Almagest , by N Expanded glossary to define and/or explain terms and Claudius Ptolemy, a Greco-Egyptian with Roman citizenship who lived concepts. in Alexandria from 90 to 160 AD. The Almagest is the earliest surviving astronomical treatise—a 600-page tome. The star charts are in tabular N Black stars on a white background, a preferred format for star form, by constellation, and the locations of the stars are described by charts.