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The Complete Abstract Booklet
First Light Science with the GTC Program and Abstracts Organizing Committees LOC – Local Organizing Committee Chris Packham (co-Chair), University of Florida Rafael Guzman (co-Chair), University of Florida Anthony Gonzalez, University of Florida Vicki Sarajedini, University of Florida Stanley Dermott, University of Florida SOC – Scientific Organizing Committee Rafael Guzman (Chair), UF, USA Jose Alberto Lopez, IAUNAM, Mexico Charles Telesco, UF, USA Elizabeth Lada, UF, USA Francisco Garzon, IAC, Spain Francisco Sanchez, IAC, Spain Itziar Aretxaga, INAOE, Mexico Jesus Gallego, UCM, Spain Jesus Gonzalez, IA-UNAM, Mexico Jian Ge, UF, USA Jordi Cepa, IAC, Spain Jose Franco, IA-UNAM, Mexico Jose Guichard, INAOE, Mexico Jose M. R. Espinosa, GTC project office, Spain Luis Colina. IEM-CSIC, Spain Marc Balcells, IAC, Spain Mariano Moles, IAA, Spain Marisa Garcia, GTC project office, Spain Stanley Dermott, UF, USA Steve Eikenberry, UF, USA Xavier Barcons, CSIC, Spain First Light Science with the GTC Sponsors First Light Science with the GTC would like to thank these organizations for their support of this meeting. Research & Graduate Programs First Light Science with the GTC General Information Date: Main Conference: Wednesday, June 28 - Friday, June 30, 2006 Post Conference Workshops: Saturday, July 1 - Tuesday, July 4, 2006 Site of the Meeting: The Biltmore Hotel 1200 Anastasia Avenue Coral Gables, FL 33134 Tel: (305) 445-1926 FAX: (305) 913-3159 Web Site: http://www.biltmorehotel.com Oral Presentations: Merrick & Stoneman Douglas (simulcast) Poster Presentations: Tuttle, Flagler & Deering Lunch: Alhambra Notice to Speakers: The speakers are requested to bring their Power Point presentation to the session room 30 minutes be- fore their sessions. -
A New Milky Way Halo Star Cluster in the Southern Galactic Sky
The Astrophysical Journal, 767:101 (6pp), 2013 April 20 doi:10.1088/0004-637X/767/2/101 C 2013. The American Astronomical Society. All rights reserved. Printed in the U.S.A. A NEW MILKY WAY HALO STAR CLUSTER IN THE SOUTHERN GALACTIC SKY E. Balbinot1,2, B. X. Santiago1,2, L. da Costa2,3,M.A.G.Maia2,3,S.R.Majewski4, D. Nidever5, H. J. Rocha-Pinto2,6, D. Thomas7, R. H. Wechsler8,9, and B. Yanny10 1 Instituto de F´ısica, UFRGS, CP 15051, Porto Alegre, RS 91501-970, Brazil; [email protected] 2 Laboratorio´ Interinstitucional de e-Astronomia–LIneA, Rua Gal. Jose´ Cristino 77, Rio de Janeiro, RJ 20921-400, Brazil 3 Observatorio´ Nacional, Rua Gal. Jose´ Cristino 77, Rio de Janeiro, RJ 22460-040, Brazil 4 Department of Astronomy, University of Virginia, Charlottesville, VA 22904-4325, USA 5 Department of Astronomy, University of Michigan, Ann Arbor, MI 48109-1042, USA 6 Observatorio´ do Valongo, Universidade Federal do Rio de Janeiro, Rio de Janeiro, RJ 20080-090, Brazil 7 Institute of Cosmology and Gravitation, University of Portsmouth, Portsmouth, Hampshire PO1 2UP, UK 8 Kavli Institute for Particle Astrophysics and Cosmology, SLAC National Accelerator Laboratory, 2575 Sand Hill Road, Menlo Park, CA 94025, USA 9 Department of Physics, Stanford University, Stanford, CA 94305, USA 10 Fermi National Laboratory, P.O. Box 500, Batavia, IL 60510-5011, USA Received 2012 October 8; accepted 2013 February 28; published 2013 April 1 ABSTRACT We report on the discovery of a new Milky Way (MW) companion stellar system located at (αJ 2000,δJ 2000) = (22h10m43s.15, 14◦5658.8). -
We Had a Great Time on the Trip. We Had Some Representatives from the Vandenberg and Santa Barbara Clubs Along with Us for the Trip
We had a great time on the trip. We had some representatives from the Vandenberg and Santa Barbara clubs along with us for the trip. The most notable thing on the trip up was a stop in La Canada Flintridge to refuel the bus and get a bite to eat. I pulled out my PST Coronado and did a little impromptu public Sun Gazing. The Sun was pretty active with a number of platform prominences as well as the ever-present flame types. A distinct sunspot group in a very disturbed area of the Sun with a bright spot had me wondering if there was a flare in progress (There wasn’t.) The patrons at the tables outside didn’t seem to object to seeing the Sun either. I had a little bit of a scare when we first got up to the gate as a couple of people who were going to meet us there were nowhere to be seen. Fortunately one of them was already on the grounds and the other showed up while we were in the Museum. Relief! As it turned out we all went on the tour of the grounds. Our tour guide Greg gave us a tour starting outside the 60” Dome. He talked about the various Solar Telescopes -the old Snow telescope which was always a non-performer because of the design of the building- too many air currents. He talked about the rivalry over the 60 and 150 ft tower solar instruments (looks like UCLA won this one over USC.) And we got a good look at the 150 ft tower. -
The Young Stellar Population of IC 1613 III
A&A 551, A74 (2013) Astronomy DOI: 10.1051/0004-6361/201219977 & c ESO 2013 Astrophysics The young stellar population of IC 1613 III. New O-type stars unveiled by GTC-OSIRIS,, M. Garcia1,2 and A. Herrero1,2 1 Instituto de Astrofísica de Canarias, C/Vía Láctea s/n, 38200 La Laguna, Tenerife, Spain e-mail: [email protected] 2 Departamento de Astrofísica, Universidad de La Laguna, Avda. Astrofísico Francisco Sánchez, s/n, 38071 La Laguna, Tenerife, Spain Received 9 July 2012 / Accepted 16 November 2012 ABSTRACT Context. Very low-metallicity massive stars are key to understanding the reionization epoch. Radiation-driven winds, chief agents in the evolution of massive stars, are consequently an important ingredient in our models of the early-Universe. Recent findings hint that the winds of massive stars with poorer metallicity than the SMC may be stronger than predicted by theory. Besides calling the paradigm of radiation-driven winds into question, this result would affect the calculated ionizing radiation and mechanical feedback of massive stars, as well as the role these objects play at different stages of the Universe. Aims. The field needs a systematic study of the winds of a large sample of very metal-poor massive stars. The sampling of spectral types is particularly poor in the very early types. This paper’s goal is to increase the list of known O-type stars in the dwarf irregular galaxy IC 1613, whose metallicity is lower than the SMC’s roughly by a factor 2. Methods. Using the reddening-free Q pseudo-colour, evolutionary masses, and GALEX photometry, we built a list of very likely O-type stars. -
1. Introduction
THE ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, 122:109È150, 1999 May ( 1999. The American Astronomical Society. All rights reserved. Printed in U.S.A. GALAXY STRUCTURAL PARAMETERS: STAR FORMATION RATE AND EVOLUTION WITH REDSHIFT M. TAKAMIYA1,2 Department of Astronomy and Astrophysics, University of Chicago, Chicago, IL 60637; and Gemini 8 m Telescopes Project, 670 North Aohoku Place, Hilo, HI 96720 Received 1998 August 4; accepted 1998 December 21 ABSTRACT The evolution of the structure of galaxies as a function of redshift is investigated using two param- eters: the metric radius of the galaxy(Rg) and the power at high spatial frequencies in the disk of the galaxy (s). A direct comparison is made between nearby (z D 0) and distant(0.2 [ z [ 1) galaxies by following a Ðxed range in rest frame wavelengths. The data of the nearby galaxies comprise 136 broad- band images at D4500A observed with the 0.9 m telescope at Kitt Peak National Observatory (23 galaxies) and selected from the catalog of digital images of Frei et al. (113 galaxies). The high-redshift sample comprises 94 galaxies selected from the Hubble Deep Field (HDF) observations with the Hubble Space Telescope using the Wide Field Planetary Camera 2 in four broad bands that range between D3000 and D9000A (Williams et al.). The radius is measured from the intensity proÐle of the galaxy using the formulation of Petrosian, and it is argued to be a metric radius that should not depend very strongly on the angular resolution and limiting surface brightness level of the imaging data. It is found that the metric radii of nearby and distant galaxies are comparable to each other. -
A Search for Pre- and Proto-Brown Dwarfs in the Dark Cloud Barnard 30 with ALMA N
A&A 597, A17 (2017) Astronomy DOI: 10.1051/0004-6361/201628510 & c ESO 2016 Astrophysics A search for pre- and proto-brown dwarfs in the dark cloud Barnard 30 with ALMA N. Huélamo1, I. de Gregorio-Monsalvo2; 3, A. Palau4, D. Barrado1, A. Bayo5; 6, M. T. Ruiz7, L. Zapata4, H. Bouy1, O. Morata8, M. Morales-Calderón1, C. Eiroa9, and F. Ménard10 1 Dpto. Astrofísica, Centro de Astrobiología (INTA-CSIC); ESAC campus, Camino bajo del Castillo s/n, Urb. Villafranca del Castillo, 28692 Villanueva de la Cañada, Spain e-mail: [email protected] 2 European Southern Observatory, 3107 Alonso de Córdova, Vitacura, Santiago, Chile 3 Joint ALMA office, 3107 Alonso de Córdova, Vitacura, Casilla 19001, Santiago 19, Chile 4 Instituto de Radioastronomía y Astrofísica, Universidad Nacional Autónoma de México, PO Box 3-72, 58090 Morelia, Michoacán, México 5 Departamento de Física y Astronomía, Facultad de Ciencias, Universidad de Valparaíso, Av. Gran Bretaña 1111, 5030 Casilla, Valparaíso, Chile 6 ICM nucleus on protoplanetary disks, Universidad de Valparaíso, Av. Gran Bretaña 1111, Valparaíso, Chile 7 Dpto. de Astronomía, Universidad de Chile, 1515 Camino del Observatorio, Santiago, Chile 8 Institute of Astronomy and Astrophysics, Academia Sinica, 11F of Astronomy-Mathematics Building, AS/NTU. No. 1, Sec. 4, Roosevelt Rd, Taipei 10617, Taiwan 9 Unidad Asociada Astro-UAM, UAM, Unidad Asociada CSIC, Universidad Autónoma de Madrid, Ctra. Colmenar km 15, 28049 Madrid, Spain 10 Institut de Planétologie et d’Astrophysique de Grenoble, UMR 5274, BP 53, 38041 Grenoble, Cedex 9, France Received 14 March 2016 / Accepted 21 September 2016 ABSTRACT Context. -
Spatial Distribution of Galactic Globular Clusters: Distance Uncertainties and Dynamical Effects
Juliana Crestani Ribeiro de Souza Spatial Distribution of Galactic Globular Clusters: Distance Uncertainties and Dynamical Effects Porto Alegre 2017 Juliana Crestani Ribeiro de Souza Spatial Distribution of Galactic Globular Clusters: Distance Uncertainties and Dynamical Effects Dissertação elaborada sob orientação do Prof. Dr. Eduardo Luis Damiani Bica, co- orientação do Prof. Dr. Charles José Bon- ato e apresentada ao Instituto de Física da Universidade Federal do Rio Grande do Sul em preenchimento do requisito par- cial para obtenção do título de Mestre em Física. Porto Alegre 2017 Acknowledgements To my parents, who supported me and made this possible, in a time and place where being in a university was just a distant dream. To my dearest friends Elisabeth, Robert, Augusto, and Natália - who so many times helped me go from "I give up" to "I’ll try once more". To my cats Kira, Fen, and Demi - who lazily join me in bed at the end of the day, and make everything worthwhile. "But, first of all, it will be necessary to explain what is our idea of a cluster of stars, and by what means we have obtained it. For an instance, I shall take the phenomenon which presents itself in many clusters: It is that of a number of lucid spots, of equal lustre, scattered over a circular space, in such a manner as to appear gradually more compressed towards the middle; and which compression, in the clusters to which I allude, is generally carried so far, as, by imperceptible degrees, to end in a luminous center, of a resolvable blaze of light." William Herschel, 1789 Abstract We provide a sample of 170 Galactic Globular Clusters (GCs) and analyse its spatial distribution properties. -
Feb BACK BAY 2019
Feb BACK BAY 2019 The official newsletter of the Back Bay Amateur Astronomers CONTENTS COMING UP Gamma Burst 2 Feb 7 BBAA Meeting Eclipse Collage 3 7:30-9PM TCC, Virginia Beach NSN Article 6 Heart Nebula 7 Feb 8 Silent Sky Club meeting 10 10-11PM Little Theatre of VB Winter DSOs 11 Contact info 16 Feb 8 Cornwatch Photo by Chuck Jagow Canon 60Da, various exposures, iOptron mount with an Orion 80ED Calendar 17 dusk-dawn The best 9 out of 3465 images taken from about 10:00 PM on the 20th Cornland Park through 2:20 AM on the 21st. Unprocessed images (only cropped). Feb 14 Garden Stars 7-8:30PM LOOKING UP! a message from the president Norfolk Botanical Gardens This month’s most talked about astronomy event has to be the total lunar Feb 16 Saturday Sun-day eclipse. The BBAA participated by supporting the Watch Party at the 10AM-1PM Chesapeake Planetarium. Anyone in attendance will tell you it was COLD, but Elizabeth River Park manageable if you wore layers, utilized the planetarium where Dr. Robert Hitt seemed to have the thermostat set to 100 degrees, and drank copious amounts Feb 23 Skywatch of the hot coffee that Kent Blackwell brewed in the back office. 6PM-10PM The event had a huge following on Facebook but with the cold Northwest River Park temperatures, we weren’t sure how many would come out. By Kent’s estimate there were between 100–200 people in attendance. Many club members set up telescopes, as well as a few members of the public too. -
The Saga of M81: Global View of a Massive Stellar Halo in Formation
Draft version October 27, 2020 Typeset using LATEX twocolumn style in AASTeX63 The Saga of M81: Global View of a Massive Stellar Halo in Formation Adam Smercina ,1, 2 Eric F. Bell ,1 Paul A. Price,3 Colin T. Slater ,2 Richard D'Souza,1, 4 Jeremy Bailin ,5 Roelof S. de Jong ,6 In Sung Jang ,6 Antonela Monachesi ,7, 8 and David Nidever 9, 10 1Department of Astronomy, University of Michigan, Ann Arbor, MI 48109, USA 2Astronomy Department, University of Washington, Box 351580, Seattle, WA 98195-1580, USA 3Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA 4Vatican Observatory, Specola Vaticana, V-00120, Vatican City State 5Department of Physics and Astronomy, University of Alabama, Box 870324, Tuscaloosa, AL 35487-0324, USA 6Leibniz-Institut f¨urAstrophysik Potsdam (AIP), An der Sternwarte 16, 14482 Potsdam, Germany 7Instituto de Investigaci´onMultidisciplinar en Ciencia y Tecnolog´ıa,Universidad de La Serena, Ra´ulBitr´an1305, La Serena, Chile 8Departamento de F´ısica y Astronom´ıa,Universidad de La Serena, Av. Juan Cisternas 1200 N, La Serena, Chile 9Department of Physics, Montana State University, P.O. Box 173840, Bozeman, MT 59717-3840 10National Optical Astronomy Observatory, 950 North Cherry Ave, Tucson, AZ 85719 (Received 31 October, 2019; Revised 31 August, 2020; Accepted 23 October, 2020) Submitted to The Astrophysical Journal ABSTRACT Recent work has shown that Milky Way-mass galaxies display an incredible range of stellar halo properties, yet the origin of this diversity is unclear. The nearby galaxy M81 | currently interacting with M82 and NGC 3077 | sheds unique light on this problem. -
Experiencing Hubble
PRESCOTT ASTRONOMY CLUB PRESENTS EXPERIENCING HUBBLE John Carter August 7, 2019 GET OUT LOOK UP • When Galaxies Collide https://www.youtube.com/watch?v=HP3x7TgvgR8 • How Hubble Images Get Color https://www.youtube.com/watch? time_continue=3&v=WSG0MnmUsEY Experiencing Hubble Sagittarius Star Cloud 1. 12,000 stars 2. ½ percent of full Moon area. 3. Not one star in the image can be seen by the naked eye. 4. Color of star reflects its surface temperature. Eagle Nebula. M 16 1. Messier 16 is a conspicuous region of active star formation, appearing in the constellation Serpens Cauda. This giant cloud of interstellar gas and dust is commonly known as the Eagle Nebula, and has already created a cluster of young stars. The nebula is also referred to the Star Queen Nebula and as IC 4703; the cluster is NGC 6611. With an overall visual magnitude of 6.4, and an apparent diameter of 7', the Eagle Nebula's star cluster is best seen with low power telescopes. The brightest star in the cluster has an apparent magnitude of +8.24, easily visible with good binoculars. A 4" scope reveals about 20 stars in an uneven background of fainter stars and nebulosity; three nebulous concentrations can be glimpsed under good conditions. Under very good conditions, suggestions of dark obscuring matter can be seen to the north of the cluster. In an 8" telescope at low power, M 16 is an impressive object. The nebula extends much farther out, to a diameter of over 30'. It is filled with dark regions and globules, including a peculiar dark column and a luminous rim around the cluster. -
The Professor Comet's Report Early Spring – April 2012
The Professor Comet’s Report 1 Mr. Justin J McCollum (BS, MS Physics) Lab Physics Coordinator Dept. of Physics Lamar University Welcome to the comet report which is a monthly article on the observations of comets by the amateur astronomy community and comet hunters from around the world! This C/2009 P1 Garradd with article is dedicated to the latest reports of available comets for Barred Spiral Galaxy NGC 4236 observations, current state of those comets, future 14 March 2011! predictions, & projections for observations in comet astronomy! Early Spring – April 2012 The Professor Comet’s Report 2 The Current Status of the Predominant Comets for Apr 2012! Comets Designation Orbital Magnitude Trend Observation Constellations Visibility (IAU – MPC) Status Visual (Range in (Night Sky Location) Period Lat.) Garradd 2009 P1 C 7.0* - 7.5 Fading 90°N – 30°S SW region of Ursa Major moving All Night SSW towards the SE region of Lynx. Giacobini - 21P P 9 – 10 Fading Poor N/A Zinner Elongation Lost in the daytime Glare! LINEAR 2011 F1 C 11 .7* Brightening 90°N – 20°S Undergoing retrograde motion All Night between Boötes and Draco thru the late Spring. Gehrels 2 78P P 12.2* Fading 60˚N - 20˚S Moving eastwards across Taurus Early Evening and progressing along the N edge of the Hyades Star Cluster! McNaught 2011 Q2 C 12.5 Fading 70˚N – Eqn. Currently in the S central region Early Morning of Andromeda moving NE between the boundary between Andromeda & Pisces. NEAT 246P/2010 V2 P 12.3* - 13 Possible 65˚N - 60˚S Undergoing retrograde motion All Night Steadiness in the E half of the N central region of Virgo until late June. -
Star Formation Relations and CO Sleds Across the J-Ladder and Redshift 3 on the ESA Herschel Space Observatory20 (Pilbratt Et Al
Draft version July 17, 2014 Preprint typeset using LATEX style emulateapj v. 5/2/11 STAR FORMATION RELATIONS AND CO SPECTRAL LINE ENERGY DISTRIBUTIONS ACROSS THE J-LADDER AND REDSHIFT T. R. Greve1, I. Leonidaki2, E. M. Xilouris2, A. Weiß3, Z.-Y. Zhang4,5, P. van der Werf6, S. Aalto7, L. Armus8, T. D´ıaz-Santos8, A.S. Evans9,10, J. Fischer11, Y. Gao12, E. Gonzalez-Alfonso´ 13, A. Harris14, C. Henkel3, R. Meijerink6,15, D. A. Naylor16 H. A. Smith17 M. Spaans15 G. J. Stacey18 S. Veilleux14 F. Walter19 Draft version July 17, 2014 ABSTRACT 0 We present FIR[50 − 300 µm]−CO luminosity relations (i.e., log LFIR = α log LCO + β) for the full CO rotational ladder from J = 1 − 0 up to J = 13 − 12 for a sample of 62 local (z ≤ 0:1) (Ultra) 11 Luminous Infrared Galaxies (LIRGs; LIR[8−1000 µm] > 10 L ) using data from Herschel SPIRE-FTS and ground-based telescopes. We extend our sample to high redshifts (z > 1) by including 35 (sub)- millimeter selected dusty star forming galaxies from the literature with robust CO observations, and sufficiently well-sampled FIR/sub-millimeter spectral energy distributions (SEDs) so that accurate FIR luminosities can be deduced. The addition of luminous starbursts at high redshifts enlarge the range of the FIR−CO luminosity relations towards the high-IR-luminosity end while also significantly increasing the small amount of mid-J/high-J CO line data (J = 5 − 4 and higher) that was available prior to Herschel. This new data-set (both in terms of IR luminosity and J-ladder) reveals linear FIR−CO luminosity relations (i.e., α ' 1) for J = 1 − 0 up to J = 5 − 4, with a nearly constant normalization (β ∼ 2).