Open Cluster Kinematics with Gaia DR2? C
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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. -
Taurus Stars Membership in the Pleiades Open Cluster
Taurus stars membership in the Pleiades open cluster Tadross, A. L., Hanna, M. A., Awadalla, N. S. National Research Institute of Astronomy & Geophysics, NRIAG, 11421 Helwan, Cairo, Egypt ABSTRACT In this paper, we study the characteristics and physical properties of the young open cluster Pleiades using Near Infra-Red, JHK pass bands. Our results have been compared with those found in new optical UBV observations. The membership validity of some variable binary stars, which are Located in Taurus constellation, and their relation with Pleiades cluster have been achieved. 1. INTRODUCTION Pleiades and Hyades are the most famous star clusters in Northern Hemisphere which can be seen by the naked eye in the constellation Taurus the bull. The star cluster surrounding Aldebaran (the eye of the bull) is the Hyades. Pleiades (NGC 1432; M45; Melotte 22; Seven Sisters) is more famous than Hyades because it is more compact cluster and easy seen, higher in the sky (~ 10 degrees from Aldebaran), see Fig 1. Pleiades is located at J (2000) α = 03h: 47m: 24s; δ = +24o: 07’: 12’’; G. long. = 166.642o and G. lat. = -23.457o. The distance to the Pleiades is an important first step in the so- called cosmic distance ladder, a sequence of distance scales for the whole universe. The optical photometry catalogs of Webda and Dais refer to Pleiades as a rich young cluster located at 135-150 pcs away from Earth. In optically observations, Pleiades covers a diameter of about 110 arcmin on the sky; its core and tidal radii are about 33 and 330 arcmins respectively. -
A Spitzer Study of Debris Disks in the Young Nearby Cluster NGC 2232
A Spitzer Study of Debris Disks In The Young Nearby Cluster NGC 2232: Icy Planets Are Common Around ∼ 1.5–3 M⊙ Stars Thayne Currie1, Peter Plavchan2, and Scott J. Kenyon1 [email protected], [email protected], [email protected] ABSTRACT We describe Spitzer IRAC and MIPS observations of the nearby 25 Myr- old open cluster NGC 2232. Combining these data with ROSAT All-Sky Survey observations, proper motions, and optical photometry/spectroscopy, we construct a list of highly probable cluster members. We identify 1 A-type star, HD 45435, with definite excess emission at 4.5–24 µm indicative of debris from terrestrial planet formation. We also identify 2–4 late-type stars with possible 8 µm excesses, and 8 early-type stars with definite 24 µm excesses. Constraints on the dust luminosity and temperature suggest that the detected excesses are produced by debris disks. From our sample of B and A stars, stellar rotation appears correlated with 24 µm excess, a result expected if massive primordial disks evolve into massive debris disks. To explore the evolution of the frequency and magnitude of debris around A-type stars, we combine our results with data for other young clusters. The frequency of debris disks around A-type stars appears to increase from ∼ 25% at 5 Myr to ∼ 50–60% at 20–25 Myr. Older A-type stars have smaller debris disk frequencies: ∼ 20% at 50–100 Myr. For these ages, the typical level of debris emission rises from 5–20 Myr and then declines. Because 24 µm dust emission probes icy planet formation around A-type stars, our results suggest that the frequency of icy planet formation is ηi & 0.5–0.6. -
February 14, 2015 7:00Pm at the Herrett Center for Arts & Science Colleagues, College of Southern Idaho
Snake River Skies The Newsletter of the Magic Valley Astronomical Society www.mvastro.org Membership Meeting President’s Message Saturday, February 14, 2015 7:00pm at the Herrett Center for Arts & Science Colleagues, College of Southern Idaho. Public Star Party Follows at the It’s that time of year when obstacles appear in the sky. In particular, this year is Centennial Obs. loaded with fog. It got in the way of letting us see the dance of the Jovian moons late last month, and it’s hindered our views of other unique shows. Still, members Club Officers reported finding enough of a clear sky to let us see Comet Lovejoy, and some great photos by members are popping up on the Facebook page. Robert Mayer, President This month, however, is a great opportunity to see the benefit of something [email protected] getting in the way. Our own Chris Anderson of the Herrett Center has been using 208-312-1203 the Centennial Observatory’s scope to do work on occultation’s, particularly with asteroids. This month’s MVAS meeting on Feb. 14th will give him the stage to Terry Wofford, Vice President show us just how this all works. [email protected] The following weekend may also be the time the weather allows us to resume 208-308-1821 MVAS-only star parties. Feb. 21 is a great window for a possible star party; we’ll announce the location if the weather permits. However, if we don’t get that Gary Leavitt, Secretary window, we’ll fall back on what has become a MVAS tradition: Planetarium night [email protected] at the Herrett Center. -
Astronomy 2008 Index
Astronomy Magazine Article Title Index 10 rising stars of astronomy, 8:60–8:63 1.5 million galaxies revealed, 3:41–3:43 185 million years before the dinosaurs’ demise, did an asteroid nearly end life on Earth?, 4:34–4:39 A Aligned aurorae, 8:27 All about the Veil Nebula, 6:56–6:61 Amateur astronomy’s greatest generation, 8:68–8:71 Amateurs see fireballs from U.S. satellite kill, 7:24 Another Earth, 6:13 Another super-Earth discovered, 9:21 Antares gang, The, 7:18 Antimatter traced, 5:23 Are big-planet systems uncommon?, 10:23 Are super-sized Earths the new frontier?, 11:26–11:31 Are these space rocks from Mercury?, 11:32–11:37 Are we done yet?, 4:14 Are we looking for life in the right places?, 7:28–7:33 Ask the aliens, 3:12 Asteroid sleuths find the dino killer, 1:20 Astro-humiliation, 10:14 Astroimaging over ancient Greece, 12:64–12:69 Astronaut rescue rocket revs up, 11:22 Astronomers spy a giant particle accelerator in the sky, 5:21 Astronomers unearth a star’s death secrets, 10:18 Astronomers witness alien star flip-out, 6:27 Astronomy magazine’s first 35 years, 8:supplement Astronomy’s guide to Go-to telescopes, 10:supplement Auroral storm trigger confirmed, 11:18 B Backstage at Astronomy, 8:76–8:82 Basking in the Sun, 5:16 Biggest planet’s 5 deepest mysteries, The, 1:38–1:43 Binary pulsar test affirms relativity, 10:21 Binocular Telescope snaps first image, 6:21 Black hole sets a record, 2:20 Black holes wind up galaxy arms, 9:19 Brightest starburst galaxy discovered, 12:23 C Calling all space probes, 10:64–10:65 Calling on Cassiopeia, 11:76 Canada to launch new asteroid hunter, 11:19 Canada’s handy robot, 1:24 Cannibal next door, The, 3:38 Capture images of our local star, 4:66–4:67 Cassini confirms Titan lakes, 12:27 Cassini scopes Saturn’s two-toned moon, 1:25 Cassini “tastes” Enceladus’ plumes, 7:26 Cepheus’ fall delights, 10:85 Choose the dome that’s right for you, 5:70–5:71 Clearing the air about seeing vs. -
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A&A 453, 101–119 (2006) Astronomy DOI: 10.1051/0004-6361:20053894 & c ESO 2006 Astrophysics On the difference between nuclear and contraction ages, W. Lyra1,2,3,A.Moitinho4,N.S.vanderBliek1,andJ.Alves5 1 Cerro Tololo Interamerican Observatory, Casilla 603 La Serena, Chile 2 Observatório do Valongo/UFRJ, Ladeira do Pedro Antônio 43, 20080-090 Rio de Janeiro, Brazil 3 Department of Astronomy and Space Physics, Uppsala Astronomical Observatory, Box 515, 751 20 Uppsala, Sweden e-mail: [email protected] 4 Observatório Astronómico de Lisboa, Tapada da Ajuda, 1349-018 Lisbon, Portugal 5 European Southern Observatory, Karl-Schwarzschild 2, 85748 Garching, Germany Received 23 July 2005 / Accepted 20 February 2006 ABSTRACT Context. Ages derived from low mass stars still contracting onto the main sequence often differ from ages derived from the high mass ones that have already evolved away from it. Aims. We investigate the general claim of disagreement between these two independent age determinations by presenting UBVRI pho- tometry for the young galactic open clusters NGC 2232, NGC 2516, NGC 2547 and NGC 4755, spanning the age range ∼10–150 Myr Methods. We derived reddenings, distances, and nuclear ages by fitting ZAMS and isochrones to color–magnitudes and color–color di- agrams. To derive contraction ages, we used four different pre-main sequence models, with an empirically calibrated color-temperature relation to match the Pleiades cluster sequence. Results. When exclusively using the V vs. V − I color–magnitude diagram and empirically calibrated isochrones, there is consistency between nuclear and contraction ages for the studied clusters. -
The Outermost Hii Regions of Nearby Galaxies
THE OUTERMOST HII REGIONS OF NEARBY GALAXIES by Jessica K. Werk A dissertation submitted in partial fulfillment of the requirements for the degree of Doctor of Philosophy (Astronomy and Astrophysics) in The University of Michigan 2010 Doctoral Committee: Professor Mario L. Mateo, Co-Chair Associate Professor Mary E. Putman, Co-Chair, Columbia University Professor Fred C. Adams Professor Lee W. Hartmann Associate Professor Marion S. Oey Professor Gerhardt R. Meurer, University of Western Australia Jessica K. Werk Copyright c 2010 All Rights Reserved To Mom and Dad, for all your love and encouragement while I was taking up space. ii ACKNOWLEDGMENTS I owe a deep debt of gratitude to a long list of individuals, institutions, and substances that have seen me through the last six years of graduate school. My first undergraduate advisor in Astronomy, Kathryn Johnston, was also my first Astronomy Professor. She piqued my interest in the subject from day one with her enthusiasm and knowledge. I don’t doubt that I would be studying something far less interesting if it weren’t for her. John Salzer, my next and last undergraduate advisor, not only taught me so much about observing and organization, but also is responsible for convincing me to go on in Astronomy. Were it not for John, I’d probably be making a lot more money right now doing something totally mind-numbing and soul-crushing. And Laura Chomiuk, a fellow Wesleyan Astronomy Alumnus, has been there for me through everything − problem sets and personal heartbreak alike. To know her as a friend, goat-lover, and scientist has meant so much to me over the last 10 years, that confining my gratitude to these couple sentences just seems wrong. -
Interstellar Extinction in the Direction of Young Open Star Clusters
ISSN (Online) 2393-8021 ISSN (Print) 2394-1588 IARJSET International Advanced Research Journal in Science, Engineering and Technology Vol. 6, Issue 5, May 2019 Interstellar Extinction in the Direction of Young Open Star Clusters Alok K. Durgapal* Center of Advanced Study, Department of Physics, D. S. B. Campus, Kumaun University Nainital, India Abstract: The total to selective extinction law in optical and near-IR wavelengths for twenty young open star clusters namely Berkeley 7, Collinder 69, Hogg 10, NGC 2362, Czernik 43, NGC 6530, NGC 6871, Bochum 10, Haffner 18, IC 4996, NGC 2384, NGC 6193, NGC 6618, NGC 7160, Collinder 232, Haffner 19, NGC 2401, NGC 6231, NGC 6823, NGC 7380 have been studied. It is found that fifteen clusters follow normal extinction law and five clusters show an anomalous behavior. Keywords: Star cluster: Reddening, interstellar dust- Interstellar extinction I. INTRODUCTION The interstellar dust which is remnant of star formation process can transmit and redirect the light of stars ([2]). As a result it becomes very difficult to determine accurate distances and magnitudes of astronomical objects ([11]); to overcome this difficulty we must have knowledge of composition of interstellar dust in every line of sight. The interstellar extinction is caused either by general interstellar medium (ISM) or by localized region of higher mean density ([9], [15]). Study of interstellar extinction provides information about components of the molecular cloud from which a star was formed. Young stars contain dust around them so young open star clusters are the ideal objects for extinction study ([5], [8], [10], [16], [17]). First started with Trumpler in 1920 and then many investigators studied extinction in the Galaxy. -
Arxiv:2012.05245V2 [Astro-Ph.GA] 5 May 2021
Draft version May 6, 2021 Typeset using LATEX twocolumn style in AASTeX63 Charting the Galactic acceleration field I. A search for stellar streams with Gaia DR2 and EDR3 with follow-up from ESPaDOnS and UVES Rodrigo Ibata 1 | Khyati Malhan 2 | Nicolas Martin 1, 3 | Dominique Aubert1 | Benoit Famaey 1 | Paolo Bianchini 1 | Giacomo Monari 1 | Arnaud Siebert 1 | Guillaume F. Thomas 4, 5 | Michele Bellazzini 6 | Piercarlo Bonifacio7 | Elisabetta Caffau7 | Florent Renaud 8 | arXiv:2012.05245v2 [astro-ph.GA] 5 May 2021 1Universit´ede Strasbourg, CNRS, Observatoire astronomique de Strasbourg, UMR 7550, F-67000 Strasbourg, France 2The Oskar Klein Centre, Department of Physics, Stockholm University, AlbaNova, SE-10691 Stockholm, Sweden 3Max-Planck-Institut f¨urAstronomie, K¨onigstuhl17, D-69117, Heidelberg, Germany 4Instituto de Astrof´ısica de Canarias, E-38205 La Laguna, Tenerife, Spain 5Universidad de La Laguna, Dpto. Astrof´ısica, E-38206 La Laguna, Tenerife, Spain 6INAF - Osservatorio di Astrofisica e Scienza dello Spazio, via Gobetti 93/3, I-40129 Bologna, Italy 7GEPI, Observatoire de Paris, Universit´ePSL, CNRS, 5 Place Jules Janssen, 92190 Meudon, France 8Department of Astronomy and Theoretical Physics, Lund Observatory, Box 43, 221 00 Lund, Sweden Corresponding author: Rodrigo Ibata [email protected] 2 Ibata et al. Submitted to ApJ ABSTRACT We present maps of the stellar streams detected in the Gaia Data Release 2 (DR2) and Early Data Release 3 (EDR3) catalogs using the STREAMFINDER algorithm. We also report the spectroscopic follow-up of the brighter DR2 stream members obtained with the high-resolution CFHT/ESPaDOnS and VLT/UVES spectrographs as well as with the medium-resolution NTT/EFOSC2 spectrograph. -
Übersicht NGC-Objektauswahl Cepheus Zur Übersichtskarte
NGC-Objektauswahl Cepheus NGC 40 NGC 7055 NGC 7354 NGC 188 NGC 7076 NGC 7380 NGC 1184 NGC 7129 NGC 7419 NGC 1544 NGC 7139 NGC 7423 NGC 2276 NGC 7142 NGC 7429 NGC 2300 NGC 7160 NGC 7510 NGC 6939 NGC 7226 NGC 7538 NGC 6949 NGC 7235 NGC 7708 NGC 6951 NGC 7261 NGC 7762 NGC 7023 NGC 7281 NGC 7822 Sternbild- Übersicht Zur Objektauswahl: Nummer anklicken Zur Übersichtskarte: Objekt anklicken Sternbildübersicht Auswahl NGC 40_7708 Aufsuchkarte Auswahl NGC 188_Aufsuchkarte 2 UMi 2 Auswahl NGC 1184 Aufsuchkarte Auswahl NGC 1544_2276_2300 Aufsuchkarte Auswahl NGC 6939 Aufsuchkarte Auswahl NGC 6949_6951 Aufsuchkarte Auswahl NGC 7023 Aufsuchkarte Auswahl NGC 7055 Aufsuchkarte Auswahl NGC 7076 Aufsuchkarte Auswahl NGC 7129_7142 Aufsuchkarte Auswahl NGC 7139_7160 Aufsuchkarte Auswahl NGC 7226_7235 Aufsuchkarte Auswahl N 7261_7281 Aufsuchkarte Auswahl NGC 7354_7419_7429_7510_7538 Aufsuchkarte Auswahl NGC 7380_7423 Aufsuchkarte Auswahl NGC 7762_7822 Aufsuchkarte Auswahl NGC 40 Übersichtskarte Aufsuch- Auswahl karte NGC 188 Übersichtskarte Aufsuch- Auswahl karte NGC 1184 Übersichtskarte Aufsuch- Auswahl karte NGC 1544 Übersichtskarte Aufsuch- Auswahl karte N 2276_N 2300 Übersichtskarte Aufsuch- Auswahl karte NGC 6939 Übersichtskarte Aufsuch- Auswahl karte NGC 6949 Übersichtskarte Aufsuch- Auswahl karte NGC 6951 Übersichtskarte Aufsuch- Auswahl karte NGC 7023 Übersichtskarte Aufsuch- Auswahl karte NGC 7055 Übersichtskarte Aufsuch- Auswahl karte NGC 7076 Übersichtskarte Aufsuch- Auswahl karte NGC 7129_7142 Übersichtskarte Aufsuch- Auswahl karte NGC 7139 -
A Case Study of the Galactic H Ii Region M17 and Environs: Implications for the Galactic Star Formation Rate
A Case Study of the Galactic H ii Region M17 and Environs: Implications for the Galactic Star Formation Rate by Matthew Samuel Povich A dissertation submitted in partial fulfillment of the requirements for the degree of Doctor of Philosophy (Astronomy) at the University of Wisconsin – Madison 2009 ii Abstract Determinations of star formation rates (SFRs) in the Milky Way and other galaxies are fundamentally based on diffuse emission tracers of ionized gas, such as optical/near-infrared recombination lines, far- infrared continuum, and thermal radio continuum, that are sensitive only to massive OB stars. OB stars dominate the ionization of H II regions, yet they make up <1% of young stellar populations. SFRs therefore depend upon large extrapolations over the stellar initial mass function (IMF). The primary goal of this Thesis is to obtain a detailed census of the young stellar population associated with a bright Galactic H II region and to compare the resulting star formation history with global SFR tracers. The main SFR tracer considered is infrared continuum, since it can be used to derive SFRs in both the Galactic and extragalactic cases. I focus this study on M17, one of the nearest giant H II regions to the Sun (d =2.1kpc),fortwo reasons: (1) M17 is bright enough to serve as an analog of observable extragalactic star formation regions, and (2) M17 is associated with a giant molecular cloud complex, ∼100 pc in extent. The M17 complex is a significant star-forming structure on the Galactic scale, with a complicated star formation history. This study is multiwavelength in nature, but it is based upon broadband mid-infrared images from the Spitzer/GLIMPSE survey and complementary infrared Galactic plane surveys. -
When Do Stalled Stars Resume Spinning Down? Advancing Gyrochronology with Ruprecht 147
The Astrophysical Journal, 904:140 (40pp), 2020 December 1 https://doi.org/10.3847/1538-4357/abbf58 © 2020. The Author(s). Published by the American Astronomical Society. When Do Stalled Stars Resume Spinning Down? Advancing Gyrochronology with Ruprecht 147 Jason Lee Curtis1,2 , Marcel A. Agüeros1 , Sean P. Matt3 , Kevin R. Covey4 , Stephanie T. Douglas5 , Ruth Angus1,2,6 , Steven H. Saar5 , Ann Marie Cody7 , Andrew Vanderburg5,8 , Nicholas M. Law9 , Adam L. Kraus8 , David W. Latham5 , Christoph Baranec10 , Reed Riddle11 , Carl Ziegler12 , Mikkel N. Lund13 , Guillermo Torres5 , Søren Meibom5, Victor Silva Aguirre13 , and Jason T. Wright14 1 Department of Astronomy, Columbia University, 550 West 120th Street, New York, NY 10027, USA; [email protected] 2 Department of Astrophysics, American Museum of Natural History, Central Park West, New York, NY, USA 3 University of Exeter, Department of Physics & Astronomy, Stocker Road, Exeter, EX4 4QL, UK 4 Department of Physics & Astronomy, Western Washington University, Bellingham, WA 98225-9164, USA 5 Center for Astrophysics, Harvard & Smithsonian, 60 Garden Street, Cambridge, MA 02138, USA 6 Center for Computational Astrophysics, Flatiron Institute, 162 5th Avenue, Manhattan, NY, USA 7 Bay Area Environmental Research Institute, 625 2nd Street, Ste. 209, Petaluma, CA 94952, USA 8 Department of Astronomy, The University of Texas at Austin, Austin, TX 78712, USA 9 Department of Physics and Astronomy, University of North Carolina, Chapel Hill, NC 27599, USA 10 Institute for Astronomy, University of Hawai‘iatMānoa, 640 N. A‘ohōkū Pl., Hilo, HI 96720-2700, USA 11 Division of Physics, Mathematics, and Astronomy, California Institute of Technology, Pasadena, CA 91125, USA 12 Dunlap Institute for Astronomy and Astrophysics, University of Toronto, 50 St.