DOCSLIB.ORG

The Messenger

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text

Load more

Recent progress on the E-ELT The Messenger New image catalogue of planetary nebulae Massive star spectroscopy with X-shooter Renewable energy plans for Paranal No. 148 – June 2012 June – 148 No. Telescopes and Instrumentation Recent Progress Towards the European Extremely Large Telescope (E-ELT) Alistair McPherson1 cepted by the ESO Council and aw aits adopted by the ESO Council as the base- Roberto Gilmozzi1 the decision on the start of construction. line for the new 39-metre E-ELT. Jason Spyromilio1 Markus Kissler-Patig1 Suzanne Ramsay1 The European Extremely Large Telescope Science capabilities (E-ELT) design has evolved significantly since the last report in The Messenger A primary concern with respect to the 1 ESO (Spyromilio et al., 2008) and here we aim new baseline for the telescope was to update the community on the activities its impact on the scientific capabilities. within the E-ELT Project Office during The E-ELT Science Office, together ESO contributors to this work include: the past few years. The construction pro- with the Science Working Group studied Jose Antonio Abad, Luigi Andolfato, Robin Arsenault, posal prepared for the ESO Council the impact on the science of the various Joana Ascenso, Pablo Barriga, Bertrand Bauvir, Henri Bonnet, Martin Brinkmann, Enzo Brunetto, has been widely publicised and is availa- modifications to the baseline design 1 3 Mark Casali, Marc Cayrel, Gianluca Chiozzi, Richard ble on the ESO website . using the Design Reference Mission and Clare, Fernando Comerón, Laura Comendador Design Reference Science Cases4 as Frutos, Ralf Conzelmann, Bernard Delabre, Alain In the second half of 2010, the E-ELT benchmarks for the evaluation. Delorme, Canio Dichirico, Philippe Dierickx, Martin Dimmler, Mark Downing, Toomas Erm, Michael programme underwent a series of techni- Esselborn, Robert Frahm, Christoph Frank, Enrico cal and managerial reviews that pro- The diameter of the primary mirror is Fedrigo, Giorgio Filippi, Peet Fourie, Fernando Gago, vided a strong endorsement of the con- the most fundamental and most impor- Paolo Ghiretti, Frederic Gonte, Juan-Carlos struction project. The activities under- tant characteristic of any telescope Gonzales, Serge Guniat, Carlos Guirao, Stephane Guisard, Juan-Pablo Haddad, Wolfgang Hacken- taken during the phase B (2007–2010) system, but particularly for an adaptive berg, Volker Heinz, Renate Hinterschuster, Ronald were thoroughly reviewed by a board of optics assisted telescope, as it deter- Holzlöhner, Richard Hook, Norbert Hubin, Lisselotte external experts in September 2010 mines both its diffraction-limited spatial Jochum, Andreas Jost, Noé Kains, Dimitrios (see Kissler-Patig, 2010). The executive resolution as well as its photon-collecting Kalaitzoglou, Robert Karban, Markus Kasper, Hans- Ulrich Käufl, Lothar Kern, Mario Kiekebusch, Franz summary of the board report has been power. These properties may combine 2 Koch, Bertrand Koehler, Johann Kolb, Nick Korn- available for some time . The short differently depending on the scientific weibel, Maximilian Kraus, Paolo La Penna, Miska version is that “it [was] the unanimous goal, as well as the observational and LeLouarn, Samuel Lévêque, Stefan Lewis, Jochen conclusion of the review board that the astrophysical circumstances. The result Liske, Jean-Louis Lizon, Gianluca Lombardi, Antonio Longinotti, Fernando Luco, Christian Lucuix, Pierre- technical maturity of the design of the is that there can be many different Yves Madec, Enrico Marchetti, Juan Marrero, Javier E-ELT was sufficient to warrant the pro- ways in which a given science case may Marti, Jorge Melnick, Katia Montironi, Christian gramme entering the construction depend on the diameter. Muckle, Michael Mueller, Julio Navarette, Helène phase”. Moreover, the “E-ELT budget was Neuville, Lothar Noethe, Paolo Padovani, Luca Pasquini, Jérôme Paufique, Lorenzo Pettazzi, Marco highly cost-effective” and the “FEED At the highest level we may distinguish Quattri, Jutta Quentin, Andrea Richichi, Robert methodology had been highly effective in between the following three classes Ridings, Mark Robinson, Michael Rosa, Stefan generating reliable cost estimates” (for a of science cases: (i) cases where science Sandrock, Pierre Sansgasset, Marc Sarazin, Michael definition of FEED see below p. 8). is irretrievably lost by reducing the tele- Schneermann, Dominik Schneller, Babak Sedghi, Ralf Siebenmorgen, Isabelle Surdej, Arek Swat, scope diameter; (ii) cases where the loss Donald Tait, Roberto Tamai, Arno van Kesteren, Elise However, the final cost estimate at the of telescope diameter can be compen- Vernet, Joël Vernet, Gianluca Verzichelli, Anders end of phase B was € 200 million above sated for by increasing the observing Wallander, Yves Wesse, Natalia Yaitskova, Michele the top end of the target. The project was time or adjusting some other observa- Zamparelli. asked to consider whether any significant tional parameter; (iii) cases that are not cost savings could be delivered without affected by the reduction of the telescope The European Extremely Large Tele- compromising the scientific capabilities of diameter at all. scope (E-ELT) has evolved over the the telescope. Unfortunately the answer last few years since the phase B review to this question was no. Some reduction The unique spatial resolution of the E-ELT of the 42-metre design. While the in scope from the 42-metre aperture is one of its defining characteristics and design was strongly endorsed, the cost would be necessary. On the other hand, hence it is not surprising that many of the exceeded the maximum envelope and following a four-year design development science cases that have been proposed a re-baselining was implemented by phase the project was also aware of for the E-ELT aim to exploit this feature. the Project Office. The extent and rami- areas where technical and programmatic All cases that require the E-ELT resolution fications of the new design are outlined risks existed. Realistic funding scenarios to disentangle their targets from other including scientific, engineering and gave an earliest possible start for the nearby sources will be forced to adopt managerial aspects. Prototyping activi- project in 2012 and therefore there was less demanding goals for the 39-metre ties of some of the components are time to work on mitigating those risks. E-ELT than originally envisaged for the described and the first light instruments The Project Office undertook to explore 42-metre design. This observational sce- have been selected. The new baseline cost saving and risk mitigation options nario encompasses a vast range of sci- for the 39-metre E-ELT has been ac­­ during 2011. These changes have been ence cases, and prominent examples 2 The Messenger 148 – June 2012 include the direct detection of exoplanets independent of diameter for the specific work. Reducing the cost of the dome (all high-contrast imaging applications re­­gime under consideration here, i.e. required a reduction in the overall volume depend particularly strongly on the diam- when going from the 42-metre to the occupied by the telescope and reducing eter), the study of the resolved stellar 39-metre aperture. This class does not the cost of all other components of the populations of other galaxies, and studies encompass many cases, but one promi- programme (excluding instrumentation) of supermassive black holes and their nent example is the detection of low- also required a reduction in the dimen- environments in the centre of our own mass exoplanets using the radial velocity sions of the telescope. and other galaxies. method. The 42-metre E-ELT design was based The other subcategory in this class of The overall loss of scientific efficiency on a three-mirror anastigmat used on- irretrievable loss contains cases where resulting from the reduction of the E-ELT axis with two folding flat mirrors extract- the observing time cannot arbitrarily diameter depends of course on how ing the beam to a suitable Nasmyth focus be extended, even in principle. Among the observing time will be distributed (Spyromilio et al., 2008). This design was such cases are included observations among the various science cases, each driven by the requirement for a Nasmyth of non-recurring transient events, such following different scaling laws. This is focus, that the telescope be adaptive as gamma-ray bursts (GRBs) or super- difficult to know a priori, but it is reason- and the large diameter. These three basic novae, and short recurring events with able to assume that the E-ELT will spend requirements, combined with a number very long periods between repetitions, much of its time doing science that of engineering risks (e.g., the maximum such as some eclipses or transits. In all of depends on the power of the diameter to size of the deformable mirror that was these cases the reduction of diameter the squared or fourth power, resulting in viable within cost and schedule con- will lead to a loss of signal-to-noise (S/N) an overall loss of efficiency in the range of straints), confined the parameter space. that cannot be compensated for by in­­ 20 to 35%. Our competitors have chosen more creasing the integration time. classical designs: Ritchey-Chrétien (RC) In addition to assessing the overall loss in the case of the Thirty Metre Telescope The second class of science cases con- of scientific efficiency, it was also evalu- (TMT) and Gregorian in the case of the tains those that are limited by the S/N ated whether any individual science Giant Magellan Telescope (GMT). We that is achievable on their targets, and cases are rendered completely infeasible considered whether a smaller telescope where the S/N is not dominated by by the reduction in the E-ELT diameter, would warrant completely new thinking (diameter-independent) astrophysical in the sense that the diameter is now in the optical design, but concluded that error sources or systematic uncertainties below some critical threshold value for the incorporation of adaptive optics in (astrophysical, instrumental, or other- these cases.
Recommended publications
  • Astronomy Magazine Special Issue

    Astronomy Magazine Special Issue

    γ ι ζ γ δ α κ β κ ε γ β ρ ε ζ υ α φ ψ ω χ α π χ φ γ ω ο ι δ κ α ξ υ λ τ μ β α σ θ ε β σ δ γ ψ λ ω σ η ν θ Aι must-have for all stargazers η δ μ NEW EDITION! ζ λ β ε η κ NGC 6664 NGC 6539 ε τ μ NGC 6712 α υ δ ζ M26 ν NGC 6649 ψ Struve 2325 ζ ξ ATLAS χ α NGC 6604 ξ ο ν ν SCUTUM M16 of the γ SERP β NGC 6605 γ V450 ξ η υ η NGC 6645 M17 φ θ M18 ζ ρ ρ1 π Barnard 92 ο χ σ M25 M24 STARS M23 ν β κ All-in-one introduction ALL NEW MAPS WITH: to the night sky 42,000 more stars (87,000 plotted down to magnitude 8.5) AND 150+ more deep-sky objects (more than 1,200 total) The Eagle Nebula (M16) combines a dark nebula and a star cluster. In 100+ this intense region of star formation, “pillars” form at the boundaries spectacular between hot and cold gas. You’ll find this object on Map 14, a celestial portion of which lies above. photos PLUS: How to observe star clusters, nebulae, and galaxies AS2-CV0610.indd 1 6/10/10 4:17 PM NEW EDITION! AtlAs Tour the night sky of the The staff of Astronomy magazine decided to This atlas presents produce its first star atlas in 2006.
  • Orthoptera: Tristiridae), En La Zona Costera Sur De La Región De Antofagasta

    Orthoptera: Tristiridae), En La Zona Costera Sur De La Región De Antofagasta

    Boletín del Museo Nacional de Historia Natural, Chile, 57: 133-138 (2008) REGISTRO EN ALTURA DE ENODISOMACRIS CURTIPENNIS CIGLIANO, 1989 (ORTHOPTERA: TRISTIRIDAE), EN LA ZONA COSTERA SUR DE LA REGIÓN DE ANTOFAGASTA MARIO ELGUETA¹ y CONSTANZA BARRÍA² ¹ Entomología, Museo Nacional de Historia Natural, Casilla 787, Santiago, Chile; [email protected] ² Instituto de Geografía, Universidad Católica de Chile, Av. Vicuña Mackenna 4860, Santiago, Chile. [email protected] RESUMEN Se documenta el hallazgo de ejemplares de Enodisomacris curtipennis Cigliano, 1989 (Tristiridae: Elasmoderini) a una altitud de 2.700 m en el Cerro Armazones en 24º34’53”S; 70º11’56”O (Datum PSAD 56) equivalente a 378.600 E y 7.280.850 S (UTM); este constituye un nuevo registro altitudinal y a la vez es la máxima altura reportada para esta especie. El Cerro Armazones forma parte de la sierra Vicuña Mackenna y se ubica al NE de la localidad costera de Paposo, a 37 km hacia el interior, en la zona sur de la Provincia de Antofagasta. Se entregan además algunos antecedentes del ambiente en que se encuentra este ortóptero. ————— Palabras clave: Tristiridae, Enodisomacris curtipennis, distribución geográfica. ABSTRACT A high altitude record for Enodisomacris curtipennis Cigliano, 1989 (Orthoptera: Tristiridae), in the Southern coastal area of Antofagasta Region. The grasshopper Enodisomacris curtipennis Cigliano, 1989 is reported for the first time at 2,700 meters of altitude in the Cerro Armazones, 24º34’53” S; 70º11’56” W (Datum PSAD 56) or 378.600 E; 7.280.850 S (UTM). This is the highest altitudinal record for this species. The hill belongs to the Vicuña Mackenna range and is located at NE of Paposo locality, in the Southern coastal area of Antofagasta Province of Chile.
  • 50 Years of Existence of the European Southern Observatory (ESO) 30 Years of Swiss Membership with the ESO

    50 Years of Existence of the European Southern Observatory (ESO) 30 Years of Swiss Membership with the ESO

    Federal Department for Economic Affairs, Education and Research EAER State Secretariat for Education, Research and Innovation SERI 50 years of existence of the European Southern Observatory (ESO) 30 years of Swiss membership with the ESO The European Southern Observatory (ESO) was founded in Paris on 5 October 1962. Exactly half a century later, on 5 October 2012, Switzerland organised a com- memoration ceremony at the University of Bern to mark ESO’s 50 years of existence and 30 years of Swiss membership with the ESO. This article provides a brief summary of the history and milestones of Swiss member- ship with the ESO as well as an overview of the most important achievements and challenges. Switzerland’s route to ESO membership Nearly twenty years after the ESO was founded, the time was ripe for Switzerland to apply for membership with the ESO. The driving forces on the academic side included the Universi- ty of Geneva and the University of Basel, which wanted to gain access to the most advanced astronomical research available. In 1980, the Federal Council submitted its Dispatch on Swiss membership with the ESO to the Federal Assembly. In 1981, the Federal Assembly adopted a federal decree endorsing Swiss membership with the ESO. In 1982, the Swiss Confederation filed the official documents for ESO membership in Paris. In 1982, Switzerland paid the initial membership fee and, in 1983, the first year’s member- ship contributions. High points of Swiss participation In 1987, the Federal Council issued a federal decree on Swiss participation in the ESO’s Very Large Telescope (VLT) to be built at the Paranal Observatory in the Chilean Atacama Desert.
  • Open Clusters in Gaia

    Open Clusters in Gaia

    Sede Amministrativa: Università degli Studi di Padova Dipartimento di Fisica e Astronomia “G. Galilei” Corso di Dottorato di Ricerca in Astronomia Ciclo XXX OPEN CLUSTERS IN GAIA ERA Coordinatore: Ch.mo Prof. Giampaolo Piotto Supervisore: Dr.ssa Antonella Vallenari Dottorando: Francesco Pensabene i Abstract Context. Open clusters (OCs) are optimal tracers of the Milky Way disc. They are observed at every distance from the Galactic center and their ages cover the entire lifespan of the disc. The actual OC census contain more than 3000 objects, but suffers of incom- pleteness out of the solar neighborhood and of large inhomogeneity in the parameter deter- minations present in literature. Both these aspects will be improved by the on-going space mission Gaia . In the next years Gaia will produce the most precise three-dimensional map of the Milky Way by surveying other than 1 billion of stars. For those stars Gaia will provide extremely precise measure- ment of proper motions, parallaxes and brightness. Aims. In this framework we plan to take advantage of the first Gaia data release, while preparing for the coming ones, to: i) move the first steps towards building a homogeneous data base of OCs with the high quality Gaia astrometry and photometry; ii) build, improve and test tools for the analysis of large sample of OCs; iii) use the OCs to explore the prop- erties of the disc in the solar neighborhood. Methods and Data. Using ESO archive data, we analyze the photometry and derive physical parameters, comparing data with synthetic populations and luminosity functions, of three clusters namely NGC 2225, NGC 6134 and NGC 2243.
  • Proto-Planetary Nebula Observing Guide

    Proto-Planetary Nebula Observing Guide

    Proto-Planetary Nebula Observing Guide www.reinervogel.net RA Dec CRL 618 Westbrook Nebula 04h 42m 53.6s +36° 06' 53" PK 166-6 1 HD 44179 Red Rectangle 06h 19m 58.2s -10° 38' 14" V777 Mon OH 231.8+4.2 Rotten Egg N. 07h 42m 16.8s -14° 42' 52" Calabash N. IRAS 09371+1212 Frosty Leo 09h 39m 53.6s +11° 58' 54" CW Leonis Peanut Nebula 09h 47m 57.4s +13° 16' 44" Carbon Star with dust shell M 2-9 Butterfly Nebula 17h 05m 38.1s -10° 08' 33" PK 10+18 2 IRAS 17150-3224 Cotton Candy Nebula 17h 18m 20.0s -32° 27' 20" Hen 3-1475 Garden-sprinkler Nebula 17h 45m 14. 2s -17° 56' 47" IRAS 17423-1755 IRAS 17441-2411 Silkworm Nebula 17h 47m 13.5s -24° 12' 51" IRAS 18059-3211 Gomez' Hamburger 18h 09m 13.3s -32° 10' 48" MWC 922 Red Square Nebula 18h 21m 15s -13° 01' 27" IRAS 19024+0044 19h 05m 02.1s +00° 48' 50.9" M 1-92 Footprint Nebula 19h 36m 18.9s +29° 32' 50" Minkowski's Footprint IRAS 20068+4051 20h 08m 38.5s +41° 00' 37" CRL 2688 Egg Nebula 21h 02m 18.8s +36° 41' 38" PK 80-6 1 IRAS 22036+5306 22h 05m 30.3s +53° 21' 32.8" IRAS 23166+1655 23h 19m 12.6s +17° 11' 33.1" Southern Objects ESO 172-7 Boomerang Nebula 12h 44m 45.4s -54° 31' 11" Centaurus bipolar nebula PN G340.3-03.2 Water Lily Nebula 17h 03m 10.1s -47° 00' 27" PK 340-03 1 IRAS 17163-3907 Fried Egg Nebula 17h 19m 49.3s -39° 10' 37.9" Finder charts measure 20° (with 5° circle) and 5° (with 1° circle) and were made with Cartes du Ciel by Patrick Chevalley (http://www.ap-i.net/skychart) Images are DSS Images (blue plates, POSS II or SERCJ) and measure 30’ by 30’ (http://archive.stsci.edu/cgi- bin/dss_plate_finder) and STScI Images (Hubble Space Telescope) Downloaded from www.reinervogel.net version 12/2012 DSS images copyright notice: The Digitized Sky Survey was produced at the Space Telescope Science Institute under U.S.
  • SAC's 110 Best of the NGC

    SAC's 110 Best of the NGC

    SAC's 110 Best of the NGC by Paul Dickson Version: 1.4 | March 26, 1997 Copyright °c 1996, by Paul Dickson. All rights reserved If you purchased this book from Paul Dickson directly, please ignore this form. I already have most of this information. Why Should You Register This Book? Please register your copy of this book. I have done two book, SAC's 110 Best of the NGC and the Messier Logbook. In the works for late 1997 is a four volume set for the Herschel 400. q I am a beginner and I bought this book to get start with deep-sky observing. q I am an intermediate observer. I bought this book to observe these objects again. q I am an advance observer. I bought this book to add to my collect and/or re-observe these objects again. The book I'm registering is: q SAC's 110 Best of the NGC q Messier Logbook q I would like to purchase a copy of Herschel 400 book when it becomes available. Club Name: __________________________________________ Your Name: __________________________________________ Address: ____________________________________________ City: __________________ State: ____ Zip Code: _________ Mail this to: or E-mail it to: Paul Dickson 7714 N 36th Ave [email protected] Phoenix, AZ 85051-6401 After Observing the Messier Catalog, Try this Observing List: SAC's 110 Best of the NGC [email protected] http://www.seds.org/pub/info/newsletters/sacnews/html/sac.110.best.ngc.html SAC's 110 Best of the NGC is an observing list of some of the best objects after those in the Messier Catalog.
  • Open Clusters

    Open Clusters

    Open Clusters Open clusters (also known as galactic clusters) are of tremendous importance to the science of astronomy, if not to astrophysics and cosmology generally. Star clusters serve as the "laboratories" of astronomy, with stars now all at nearly the same distance and all created at essentially the same time. Each cluster thus is a running experiment, where we can observe the effects of composition, age, and environment. We are hobbled by seeing only a snapshot in time of each cluster, but taken collectively we can understand their evolution, and that of their included stars. These clusters are also important tracers of the Milky Way and other parent galaxies. They help us to understand their current structure and derive theories of the creation and evolution of galaxies. Just as importantly, starting from just the Hyades and the Pleiades, and then going to more distance clusters, open clusters serve to define the distance scale of the Milky Way, and from there all other galaxies and the entire universe. However, there is far more to the study of star clusters than that. Anyone who has looked at a cluster through a telescope or binoculars has realized that these are objects of immense beauty and symmetry. Whether a cluster like the Pleiades seen with delicate beauty with the unaided eye or in a small telescope or binoculars, or a cluster like NGC 7789 whose thousands of stars are seen with overpowering wonder in a large telescope, open clusters can only bring awe and amazement to the viewer. These sights are available to all.
  • Atlas Menor Was Objects to Slowly Change Over Time

    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.
  • A Compendium of Distances to Molecular Clouds in the Star Formation Handbook?,?? Catherine Zucker1, Joshua S

    A Compendium of Distances to Molecular Clouds in the Star Formation Handbook?,?? Catherine Zucker1, Joshua S

    A&A 633, A51 (2020) Astronomy https://doi.org/10.1051/0004-6361/201936145 & c ESO 2020 Astrophysics A compendium of distances to molecular clouds in the Star Formation Handbook?,?? Catherine Zucker1, Joshua S. Speagle1, Edward F. Schlafly2, Gregory M. Green3, Douglas P. Finkbeiner1, Alyssa Goodman1,5, and João Alves4,5 1 Center for Astrophysics | Harvard & Smithsonian, 60 Garden St., Cambridge, MA 02138, USA e-mail: [email protected], [email protected] 2 Lawrence Berkeley National Laboratory, One Cyclotron Road, Berkeley, CA 94720, USA 3 Kavli Institute for Particle Astrophysics and Cosmology, Physics and Astrophysics Building, 452 Lomita Mall, Stanford, CA 94305, USA 4 University of Vienna, Department of Astrophysics, Türkenschanzstraße 17, 1180 Vienna, Austria 5 Radcliffe Institute for Advanced Study, Harvard University, 10 Garden St, Cambridge, MA 02138, USA Received 21 June 2019 / Accepted 12 August 2019 ABSTRACT Accurate distances to local molecular clouds are critical for understanding the star and planet formation process, yet distance mea- surements are often obtained inhomogeneously on a cloud-by-cloud basis. We have recently developed a method that combines stellar photometric data with Gaia DR2 parallax measurements in a Bayesian framework to infer the distances of nearby dust clouds to a typical accuracy of ∼5%. After refining the technique to target lower latitudes and incorporating deep optical data from DECam in the southern Galactic plane, we have derived a catalog of distances to molecular clouds in Reipurth (2008, Star Formation Handbook, Vols. I and II) which contains a large fraction of the molecular material in the solar neighborhood. Comparison with distances derived from maser parallax measurements towards the same clouds shows our method produces consistent distances with .10% scatter for clouds across our entire distance spectrum (150 pc−2.5 kpc).
  • Skytools Chart

    Skytools Chart

    22 Aquila - Scutum SkyTools 3 / Skyhound.com 7006 γ2 α IC 4997 γ1 δ ρ ε β ζ ζ Delphinus 6891 NGC 6738 ε δ γ γ NGC 6709 κ 6803 +10° ξ 6934 μ Blue Racquetball 6781 NGC 6633 β IC 4665 IC 4756 NGC 6755 θ1 Aquila θ2 Equuleus δ γ Collinder 359 6852 6790 Collinder 350 η 6760 ν Collinder 401 Phantom Streak +0° θ 6535 ι Serpens Cauda ζ λ β NGC 6704 6751 η NGC 6683 κ Wild Duck Cluster IC 1276 NGC 6664 6539 6712 ε α τ IC 4846 μ δ ζ 6517 ε M 26 ν -10° Scutum ν Saturn Nebula NGC 6625 2 NGC 6604 M 73 M72 ν α α1 Eagle Nebula Little Gem Star Queen Barnard's Galaxy γ β NGC 6605 τ h 8 υ Omega Nebula 1 M 17 52° x 34° 19h30m00.0s +00°00'00" (Skymark) Open Cl. Nebula Galaxy 8 7 6 5 4 3 2 1 Globular Cl. Dark Neb. Quasar Globule Planetary 22 Aquila - Scutum GALASSIE Sigla Nome Cost. A.R. Dec. Mv. Dim. Tipo Distanza 200/4 80/11,5 20x60 NGC 6822 Barnard's Gal. Sgr 19h 47m 58s -14° 48' 11" +9,40 13',5x12',3 IB 4,4 Mly Er 20 (dif.) Er 20 (v. c.) (v. c.) AMMASSI APERTI Sigla Nome Cost. A.R. Dec. Mv. Dim. N° Æ Distanza 200/4 80/11,5 20x60 IC 4665 Oph 17h 46m 18s +05° 43' 00" +5,30 70',0 29 1.100 ly Er 20 (det.) Er 15,5 (det.) (dif.) Cr 350 Oph 17h 48m 06s +01° 18' 00" +6,10 39',0 --- 930 ly Er 12,4 (det.) Er 20 (det.) (dif.) Cr 359 Oph 18h 01m 06s +02° 54' 00" +3,00 240',0 --- 810 ly Er 20 (det.) Er 20 (det.) (det.) NGC 6604 Ser 18h 18m 04s -12° 14' 30" +7,50 5',0 30 5.500 ly Er 20 (easy) Er 20 (easy) (det.) NGC 6605 Ser 18h 18m 21s -14° 56' 42" +6,00 15',0 12 --- Er 20 (dif.) Er 20 (cha.) (cha.) M 16 Star Queen Ser 18h 18m 48s -13° 48' 24" +6,50 6',0 60 5.700 ly Er 20 (obv.) Er 20 (easy) (easy) M 17 Sgr 18h 20m 47s -16° 10' 18" +7,30 25',0 --- 4.200 Or 6 (dif.) Er 20 (cha.) (v.
  • Characterising Open Clusters in the Solar Neighbourhood with the Tycho-Gaia Astrometric Solution? T

    Characterising Open Clusters in the Solar Neighbourhood with the Tycho-Gaia Astrometric Solution? T

    A&A 615, A49 (2018) Astronomy https://doi.org/10.1051/0004-6361/201731251 & © ESO 2018 Astrophysics Characterising open clusters in the solar neighbourhood with the Tycho-Gaia Astrometric Solution? T. Cantat-Gaudin1, A. Vallenari1, R. Sordo1, F. Pensabene1,2, A. Krone-Martins3, A. Moitinho3, C. Jordi4, L. Casamiquela4, L. Balaguer-Núnez4, C. Soubiran5, and N. Brouillet5 1 INAF-Osservatorio Astronomico di Padova, vicolo Osservatorio 5, 35122 Padova, Italy e-mail: [email protected] 2 Dipartimento di Fisica e Astronomia, Università di Padova, vicolo Osservatorio 3, 35122 Padova, Italy 3 SIM, Faculdade de Ciências, Universidade de Lisboa, Ed. C8, Campo Grande, 1749-016 Lisboa, Portugal 4 Institut de Ciències del Cosmos, Universitat de Barcelona (IEEC-UB), Martí i Franquès 1, 08028 Barcelona, Spain 5 Laboratoire d’Astrophysique de Bordeaux, Univ. Bordeaux, CNRS, UMR 5804, 33615 Pessac, France Received 26 May 2017 / Accepted 29 January 2018 ABSTRACT Context. The Tycho-Gaia Astrometric Solution (TGAS) subset of the first Gaia catalogue contains an unprecedented sample of proper motions and parallaxes for two million stars brighter than G 12 mag. Aims. We take advantage of the full astrometric solution available∼ for those stars to identify the members of known open clusters and compute mean cluster parameters using either TGAS or the fourth U.S. Naval Observatory CCD Astrograph Catalog (UCAC4) proper motions, and TGAS parallaxes. Methods. We apply an unsupervised membership assignment procedure to select high probability cluster members, we use a Bayesian/Markov Chain Monte Carlo technique to fit stellar isochrones to the observed 2MASS JHKS magnitudes of the member stars and derive cluster parameters (age, metallicity, extinction, distance modulus), and we combine TGAS data with spectroscopic radial velocities to compute full Galactic orbits.
  • The Young Cluster NGC 6604 and the Serpens OB2 Association

    The Young Cluster NGC 6604 and the Serpens OB2 Association

    Handbook of Star Forming Regions Vol. II Astronomical Society of the Pacific, c 2008 Bo Reipurth, ed. The Young Cluster NGC 6604 and the Serpens OB2 Association Bo Reipurth Institute for Astronomy, University of Hawaii 640 N. Aohoku Place, Hilo, HI 96720, USA Abstract. NGC 6604 is a young cluster in Serpens with an age of 4-5 Myr and at a distance of about 1.7 kpc. It forms the densest part of the wider Ser OB2 associa- tion, which contains about 100 OB stars. NGC 6604 lies about 65 pc above the Galactic plane, and has attracted special interest since it has produced a thermal chimney stretch- ing 200 pc out of the plane. The combined effect of winds and radiation from the many OB stars has produced a rim of dense molecular material in which second-generation star formation is currently taking place. 1. Introduction NGC 6604 is a young cluster, originally discovered by William Herschel in 1784 and listed as H VIII-15, and later catalogued by John Herschel as h3740. It is also listed as Cr 373 in the catalogue of Collinder (1931). It is located in a rich part of the Milky Way in the constellation Serpens, only about 1.5 degrees north of NGC 6611. The center of the cluster is at J2000: 18h 18.0m −12◦ 14′. The general region is seen in Figures 1 and 2. 2. The NGC 6604 Cluster - Distance and Age Early distance estimates for NGC 6604 are uncertain and vary from 0.7 kpc to 4.4 kpc; they are listed in Alter et al.