Authors for “Hubble Space Telescope Observations of Oxygen-Rich Supernova Remnants in the Magellanic Clouds
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Nebula in NGC 2264
Durham E-Theses The polarisation of the cone(IRN) Nebula in NGC 2264 Hill, Marianne C.M. How to cite: Hill, Marianne C.M. (1991) The polarisation of the cone(IRN) Nebula in NGC 2264, Durham theses, Durham University. Available at Durham E-Theses Online: http://etheses.dur.ac.uk/6098/ Use policy The full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-prot purposes provided that: • a full bibliographic reference is made to the original source • a link is made to the metadata record in Durham E-Theses • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders. Please consult the full Durham E-Theses policy for further details. Academic Support Oce, Durham University, University Oce, Old Elvet, Durham DH1 3HP e-mail: [email protected] Tel: +44 0191 334 6107 http://etheses.dur.ac.uk THE POLARISATION OF THE CONE(IRN) NEBULA IN NGC 2264 MARIANNE C. M. HILL A Thesis submitted to the University of Durham for the degree of Master of Science. The copyright of this thesis rests with the author. No quotation from it should be published without prior consent and information derived from it should be acknowledged. Department of Physics. September 1991 The copyright of this thesis rests with the author. No quotation from it should be published without his prior written consent and information derived from it should be acknowledged. -
Stars and Their Spectra: an Introduction to the Spectral Sequence Second Edition James B
Cambridge University Press 978-0-521-89954-3 - Stars and Their Spectra: An Introduction to the Spectral Sequence Second Edition James B. Kaler Index More information Star index Stars are arranged by the Latin genitive of their constellation of residence, with other star names interspersed alphabetically. Within a constellation, Bayer Greek letters are given first, followed by Roman letters, Flamsteed numbers, variable stars arranged in traditional order (see Section 1.11), and then other names that take on genitive form. Stellar spectra are indicated by an asterisk. The best-known proper names have priority over their Greek-letter names. Spectra of the Sun and of nebulae are included as well. Abell 21 nucleus, see a Aurigae, see Capella Abell 78 nucleus, 327* ε Aurigae, 178, 186 Achernar, 9, 243, 264, 274 z Aurigae, 177, 186 Acrux, see Alpha Crucis Z Aurigae, 186, 269* Adhara, see Epsilon Canis Majoris AB Aurigae, 255 Albireo, 26 Alcor, 26, 177, 241, 243, 272* Barnard’s Star, 129–130, 131 Aldebaran, 9, 27, 80*, 163, 165 Betelgeuse, 2, 9, 16, 18, 20, 73, 74*, 79, Algol, 20, 26, 176–177, 271*, 333, 366 80*, 88, 104–105, 106*, 110*, 113, Altair, 9, 236, 241, 250 115, 118, 122, 187, 216, 264 a Andromedae, 273, 273* image of, 114 b Andromedae, 164 BDþ284211, 285* g Andromedae, 26 Bl 253* u Andromedae A, 218* a Boo¨tis, see Arcturus u Andromedae B, 109* g Boo¨tis, 243 Z Andromedae, 337 Z Boo¨tis, 185 Antares, 10, 73, 104–105, 113, 115, 118, l Boo¨tis, 254, 280, 314 122, 174* s Boo¨tis, 218* 53 Aquarii A, 195 53 Aquarii B, 195 T Camelopardalis, -
GEORGE HERBIG and Early Stellar Evolution
GEORGE HERBIG and Early Stellar Evolution Bo Reipurth Institute for Astronomy Special Publications No. 1 George Herbig in 1960 —————————————————————– GEORGE HERBIG and Early Stellar Evolution —————————————————————– Bo Reipurth Institute for Astronomy University of Hawaii at Manoa 640 North Aohoku Place Hilo, HI 96720 USA . Dedicated to Hannelore Herbig c 2016 by Bo Reipurth Version 1.0 – April 19, 2016 Cover Image: The HH 24 complex in the Lynds 1630 cloud in Orion was discov- ered by Herbig and Kuhi in 1963. This near-infrared HST image shows several collimated Herbig-Haro jets emanating from an embedded multiple system of T Tauri stars. Courtesy Space Telescope Science Institute. This book can be referenced as follows: Reipurth, B. 2016, http://ifa.hawaii.edu/SP1 i FOREWORD I first learned about George Herbig’s work when I was a teenager. I grew up in Denmark in the 1950s, a time when Europe was healing the wounds after the ravages of the Second World War. Already at the age of 7 I had fallen in love with astronomy, but information was very hard to come by in those days, so I scraped together what I could, mainly relying on the local library. At some point I was introduced to the magazine Sky and Telescope, and soon invested my pocket money in a subscription. Every month I would sit at our dining room table with a dictionary and work my way through the latest issue. In one issue I read about Herbig-Haro objects, and I was completely mesmerized that these objects could be signposts of the formation of stars, and I dreamt about some day being able to contribute to this field of study. -
Observing Variable Nebulae Variable Nebulae Available to Amateur Observers Seen Again Until 1890 When It Was Barely Recovered by E
THE BAA OBSERVERS’ WORKSHOPS Cambridge Winchester York 2003 February 15 2003 April 26 2003 September 6 Dr Nick Hewitt continues our series of extracts from the talks at the Observers’ Workshops. Observing Workshop No. 1: The Institute of Astronomy, variable nebulae Cambridge 2003 February 15 by Nick Hewitt mechanisms are different and amateur Hubble while at Mount Wilson Observa- Introduction observation is difficult. tory. In 1916 he compared past photo- YSOs are formed in the molecular graphic plates of the nebula that showed Most deep sky observers enjoy their clouds to be found in the spiral arms in changes in brightness and dark areas on Universe for the aesthetic beauty on the Milky Way galaxy. We can only see the ‘fan’ of the nebula that did not display, and to strive to pull out detail in the nearer examples, though presumably correspond to the variations in R their quarry, or capture the gossamer the phenomenon is common. But many Monocerotis itself. This prompted Carl detail by drawing, by photographs, or YSOs are obscured in the dusty and Lampland, a pioneer astrophotographer at more recently using CCDs. Only a gaseous regions of the Galaxy. The Lowell Observatory, to take over 1000 minority consider doing real science and nearest dark molecular clouds are in photographs of the nebula between 1919 pursuing any of the deep sky observing Taurus, and indeed many YSOs are to be and 1951. Much was gleaned from this projects that the British Astronomical found there, but anywhere where there is work, and his observations are still used Association promotes. -
Astronomy Magazine 2011 Index Subject Index
Astronomy Magazine 2011 Index Subject Index A AAVSO (American Association of Variable Star Observers), 6:18, 44–47, 7:58, 10:11 Abell 35 (Sharpless 2-313) (planetary nebula), 10:70 Abell 85 (supernova remnant), 8:70 Abell 1656 (Coma galaxy cluster), 11:56 Abell 1689 (galaxy cluster), 3:23 Abell 2218 (galaxy cluster), 11:68 Abell 2744 (Pandora's Cluster) (galaxy cluster), 10:20 Abell catalog planetary nebulae, 6:50–53 Acheron Fossae (feature on Mars), 11:36 Adirondack Astronomy Retreat, 5:16 Adobe Photoshop software, 6:64 AKATSUKI orbiter, 4:19 AL (Astronomical League), 7:17, 8:50–51 albedo, 8:12 Alexhelios (moon of 216 Kleopatra), 6:18 Altair (star), 9:15 amateur astronomy change in construction of portable telescopes, 1:70–73 discovery of asteroids, 12:56–60 ten tips for, 1:68–69 American Association of Variable Star Observers (AAVSO), 6:18, 44–47, 7:58, 10:11 American Astronomical Society decadal survey recommendations, 7:16 Lancelot M. Berkeley-New York Community Trust Prize for Meritorious Work in Astronomy, 3:19 Andromeda Galaxy (M31) image of, 11:26 stellar disks, 6:19 Antarctica, astronomical research in, 10:44–48 Antennae galaxies (NGC 4038 and NGC 4039), 11:32, 56 antimatter, 8:24–29 Antu Telescope, 11:37 APM 08279+5255 (quasar), 11:18 arcminutes, 10:51 arcseconds, 10:51 Arp 147 (galaxy pair), 6:19 Arp 188 (Tadpole Galaxy), 11:30 Arp 273 (galaxy pair), 11:65 Arp 299 (NGC 3690) (galaxy pair), 10:55–57 ARTEMIS spacecraft, 11:17 asteroid belt, origin of, 8:55 asteroids See also names of specific asteroids amateur discovery of, 12:62–63 -
March Preparing for Your Stargazing Session
Central Coast Astronomical Stargazing March Preparing for your stargazing session: Step 1: Download your free map of the night sky: SkyMaps.com They have it available for Northern and Southern hemispheres. Step 2: Print out this document and use it to take notes during your stargazing session. Step 3: Watch our stargazing video: youtu.be/YewnW2vhxpU *Image credit: all astrophotography images are courtesy of NASA & ESO unless otherwise noted. All planetarium images are courtesy of Stellarium. Main Focus for the Session: 1. Monoceros (the Unicorn) 2. Puppis (the Stern) 3. Vela (the Sails) 4. Carina (the Keel) Notes: Central Coast Astronomy CentralCoastAstronomy.org Page 1 Monoceros (the Unicorn) Monoceros, (the unicorn), meaning “one horn” from the Greek. This is a modern constellation in the northern sky created by Petrus Plancius in 1612. Rosette Nebula is an open cluster plus the surrounding emission nebula. The open cluster is actually denoted NGC 2244, while the surrounding nebulosity was discovered piecemeal by several astronomers and given multiple NGC numbers. This is an area where a cluster of young stars about 3 million years old have blown a hole in the gas and dust where they were born. Hard ultraviolet light from these young stars have excited the gases in the surrounding nebulosity, giving the red wreath-like appearance in photographs. NGC 2244 is in the center of this roughly round nebula. This cluster has a visual magnitude of 4.8 and a distance of about 4900 light years. It was discovered by William Herschel on January 24, 1784. NGC 2244 is about 24’ across and contains about 100 stars. -
Terry Adrian's Finest NGC Chart/Log System
RASC FINEST NGC No. NGC Con Type R.A. Dec m_v Size Remarks Seen Date Autumn 1 7009 Aqr PN 21:04.2 -11:02 8.3 25" !! Saturn Nebula; small bright oval 2 7293 Aqr PN 22:29.6 -20:48 6.5 12'50" !! Helix Nebula; large, diffuse; use filter 3 7331 Peg G-Sb 22:37.1 +34:25 9.5 10.7x4.0 !! large, bright spiral galaxy 4 7635 Cas EN 23:20.7 +61:12 - 15x8 Bubble Neb.; very faint; 1/2 deg SW of M52 5 7789 Cas OC 23:57.0 +56:44 6.7 16 !! 300*; faint but very rich cluster 6 185 Cas G-E0 00:39.0 +48:20 11.7 2x2 companion to M31; paired with NGC 147 7 281 Cas EN 00:52.8 +56:36 - 35x30 !! large faint nebulosity near eta Cas 8 457 Cas OC 01:19.1 +58:20 6.4 13 80*; rich; one of the best Cas clusters 9 663 Cas OC 01:46.0 +61:15 7.1 16 80*; look for NGC's 654 and 659 nearby 10 I 289 Cas PN 03:10.3 +61:19 12.3 34" dim oval smudge; use nebula filter 11 7662 And PN 23:25.9 +42:33 9.2 20" !! Blue Snowball; annular at high power 12 891 And G-Sb 02:22.6 +42:21 10 13.5x2.8 !! faint, classic edge-on with dust lane 13 253 Scl G-Scp 00:47.6 -25:17 7.1 25.1x7.4 !! very large and bright but at low altitude 14 772 Ari G-Sb 01:59.3 +19:01 10.3 7.1x4.5 diffuse spiral galaxy 15 246 Cet PN 00:47.0 -11:53 8.0 3'45" faint (closer to 11 m); dark mottling 16 936 Cet G-SBa 02:27.6 -01:09 10.1 5.2x4.4 near M77; NGC 941 in the same field 17 869/84 Per OC 02:20.0 +57:08 ~4.4 30/30 !! Double Cluster; 350*; use low mag. -
Astronomy Magazine 2020 Index
Astronomy Magazine 2020 Index SUBJECT A AAVSO (American Association of Variable Star Observers), Spectroscopic Database (AVSpec), 2:15 Abell 21 (Medusa Nebula), 2:56, 59 Abell 85 (galaxy), 4:11 Abell 2384 (galaxy cluster), 9:12 Abell 3574 (galaxy cluster), 6:73 active galactic nuclei (AGNs). See black holes Aerojet Rocketdyne, 9:7 airglow, 6:73 al-Amal spaceprobe, 11:9 Aldebaran (Alpha Tauri) (star), binocular observation of, 1:62 Alnasl (Gamma Sagittarii) (optical double star), 8:68 Alpha Canum Venaticorum (Cor Caroli) (star), 4:66 Alpha Centauri A (star), 7:34–35 Alpha Centauri B (star), 7:34–35 Alpha Centauri (star system), 7:34 Alpha Orionis. See Betelgeuse (Alpha Orionis) Alpha Scorpii (Antares) (star), 7:68, 10:11 Alpha Tauri (Aldebaran) (star), binocular observation of, 1:62 amateur astronomy AAVSO Spectroscopic Database (AVSpec), 2:15 beginner’s guides, 3:66, 12:58 brown dwarfs discovered by citizen scientists, 12:13 discovery and observation of exoplanets, 6:54–57 mindful observation, 11:14 Planetary Society awards, 5:13 satellite tracking, 2:62 women in astronomy clubs, 8:66, 9:64 Amateur Telescope Makers of Boston (ATMoB), 8:66 American Association of Variable Star Observers (AAVSO), Spectroscopic Database (AVSpec), 2:15 Andromeda Galaxy (M31) binocular observations of, 12:60 consumption of dwarf galaxies, 2:11 images of, 3:72, 6:31 satellite galaxies, 11:62 Antares (Alpha Scorpii) (star), 7:68, 10:11 Antennae galaxies (NGC 4038 and NGC 4039), 3:28 Apollo missions commemorative postage stamps, 11:54–55 extravehicular activity -
Arxiv:Astro-Ph/0611634V1 20 Nov 2006
Last edited August 28, 2006 Infrared Nebulae Around Young Stellar Objects Michael S. Connelley1 Bo Reipurth2 and Alan T. Tokunaga3 ABSTRACT We present a K-band atlas of 106 reflection nebulae, 41 of which are new discoveries. We observed these nebulae with the UH 2.2 m telescope in the course of an imaging survey of 197 objects that were selected to be nearby young Class I sources. K-band images and flux calibrated surface brightness contour plots of each nebula are presented. We found that the near-IR luminosities and physical sizes of the nebulae increase with the bolometric luminosity of the illuminating sources. Only 22 nebulae, about 10% of these candidate Class I sources, have indications of shocked H2 emission. The great variety of nebulae that we observed prevented us from classifying them based on morphology. However, we note that as the spectral index decreases, the central star is more frequently visible at K- band and the flux from the central star tends to be dominant over the flux from the nebula. For objects that have a higher spectral index, most of the K-band flux is from the reflection nebula, and the central star is less frequently visible. arXiv:astro-ph/0611634v1 20 Nov 2006 The nebula around IRAS 05450+0019 has a unique morphology, and we speculate that it may be an example of a disk shadow being projected into the surrounding cloud. We present J, H, and K-band images of this object with surface brightness contours, as well as its SED from 1.2 µm to 100 µm. -
254 — 13 February 2014 Editor: Bo Reipurth ([email protected]) List of Contents
THE STAR FORMATION NEWSLETTER An electronic publication dedicated to early stellar/planetary evolution and molecular clouds No. 254 — 13 February 2014 Editor: Bo Reipurth ([email protected]) List of Contents The Star Formation Newsletter Interview ...................................... 3 My Favorite Object ............................ 5 Editor: Bo Reipurth [email protected] Perspective ................................... 10 Technical Editor: Eli Bressert Abstracts of Newly Accepted Papers .......... 13 [email protected] Abstracts of Newly Accepted Major Reviews . 54 Technical Assistant: Hsi-Wei Yen Dissertation Abstracts ........................ 60 [email protected] New Jobs ..................................... 61 Editorial Board Meetings ..................................... 63 Summary of Upcoming Meetings ............. 66 Joao Alves Alan Boss Short Announcements ........................ 67 Jerome Bouvier New Books ................................... 68 Lee Hartmann Thomas Henning Paul Ho Jes Jorgensen Charles J. Lada Cover Picture Thijs Kouwenhoven Michael R. Meyer This image shows the blueshifted outflow cav- Ralph Pudritz ity from the embedded quadruple Class I source Luis Felipe Rodr´ıguez L1551 IRS5 based on Hα and [SII] images obtained Ewine van Dishoeck with the Subaru telescope images. Two short jets, Hans Zinnecker HH 154, are seen to emerge from the source region to the upper left. The outflow cavity has burst The Star Formation Newsletter is a vehicle for through the front of the cloud, exposing the rich fast distribution of information of interest for as- and complex Herbig-Haro shock structures within. tronomers working on star and planet formation A few faint knots from the HH 30 jet (outside the and molecular clouds. You can submit material field) are visible at the top of the image. The for the following sections: Abstracts of recently field is about 7×8 arcmin, corresponding to about accepted papers (only for papers sent to refereed 0.30×0.35 pc at the assumed distance of 150 pc. -
Stellar Reflection Nebulae
Florian Koller Stellar reflection nebulae Bachelor Thesis University of Graz Institute of Physics / Geophysics, Astrophysics und Meteorology (IGAM) Supervisor: Dr. Thorsten Ratzka Graz, September 2016 Contents 1 Abstract 4 2 Kurzbeschreibung 4 3 Basis 5 3.1 Theory . ................... 5 3.1.1 Interstellar dust and Scattering . 5 3.1.2 Stellar evolution - young stellar objects YSOs . 6 3.1.3 Herbig Haro objects . .......... 7 3.1.4 Stellar evolution- Post AGB stars . 7 3.2 Technical basis . ................ 8 3.2.1 Telescope . .............. 8 3.2.2 Camera . ............... 8 3.2.3 Filter . ................. 9 3.2.4 Signal-to-noise ratio and image display . 10 4 Measurement and optical calculations 13 4.1 Observation on 17 March 2016 . 13 4.2 Observation on 14 April 2016 . 13 4.3 Observation on 20 April 2016 . 13 4.4 Observation on 21 May 2016 . 14 4.5 Information on the location of the observatory . 14 4.6 Determination of the optical layout and seeing conditions . 15 4.6.1 Field of view . 15 4.6.2 Determining the seeing . 18 4.6.3 Spatial resolution . 19 5 Data reduction 21 6 Analysis 24 6.1 NGC 1555, Hind’s Nebula . 24 6.2 AB Aur . .................... 26 6.3 Holoea . ................... 27 6.4 FU Ori . .................... 29 6.5 NGC 2261, Hubble’s Variable Nebula . 31 6.6 HK Ori . .................... 34 6.7 CED 62 . .................... 35 6.8 RY Tau . ................... 35 6.9 XY Per . .................... 36 6.10 V633 Cas and V376 Cas . 37 6.11 V628 Cas . 39 6.12 Parsamian 21 . 40 6.13 PV Cep, Gyulbudaghian’s Nebula . -
Spitzer Approved Galactic Spitzer Approved Galactic
Printed_by_SSC Mar 25, 10 16:33Spitzer_Approved_Galactic Page 1/847 Mar 25, 10 16:33Spitzer_Approved_Galactic Page 2/847 Spitzer Space Telescope − Archive Research Proposal #20309 Spitzer Space Telescope − Archive Research Proposal #30144 PAH Emission Features in the 15 to 20 Micron Region: Emitting to the Beat of a Diamonds are a PAHs Best Friend Different Drummer Principal Investigator: Louis Allamandola Principal Investigator: Louis Allamandola Institution: NASA Ames Research Center Institution: NASA Ames Research Center Technical Contact: Louis Allamandola, NASA Ames Research Center Technical Contact: Louis Allamandola, NASA Ames Research Center Co−Investigators: Co−Investigators: Andrew Mattioda, SETI Andrew Mattioda, SETI Institute and NASA Ames Els Peeters, SETI Els Peeters, NASA Ames Research Center Douglas Hudgins, NASA Ames Research Center Douglas Hudgins, NASA Ames Research Center Alexander Tielens, NASA Ames Research Center Xander Tielens, Kapteyn Institute, The Netherlands Charles Bauschlicher, Jr., NASA Ames Research Center Charlie Bauschlicher, Jr., NASA Ames Research Center Science Category: ISM Science Category: ISM Dollars Approved: 56727.0 Dollars Approved: 72000.0 Abstract: Abstract: The mid−IR spectroscopic capabilities and unprecedented sensitivity of the Spitzer has added a new complex of bands near 17 um to the PAH emission band Spitzer Space Telescope has shown that the ubiquitious infrared (IR) emission family. This 17 um band complex, the second most intense of the PAH features, features can be used as probes of many galactic and extragalactic objects. carries unique information about the emitting species. Because these bands arise These features, formerly called the Unidentified Infrared (UIR) Bands, are now from drumhead vibrations of the hexagonal carbon skeleton, they carry generally attributed to the vibrational emission from polycyclic aromatic information directly related to PAH shape, size, and charge.