The Ancient Starry Ship
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The Messenger
10th anniversary of VLT First Light The Messenger The ground layer seeing on Paranal HAWK-I Science Verification The emission nebula around Antares No. 132 – June 2008 –June 132 No. The Organisation The Perfect Machine Tim de Zeeuw a groundbased spectroscopic comple thousand each semester, 800 of which (ESO Director General) ment to the Hubble Space Telescope. are for Paranal. The User Portal has Italy and Switzerland had joined ESO in about 4 000 registered users and 1981, enabling the construction of the the archive contains 74 TB of data and This issue of the Messenger marks the 3.5m New Technology Telescope with advanced data products. tenth anniversary of first light of the Very pioneering advances in active optics, Large Telescope. It is an excellent occa crucial for the next step: the construction sion to look at the broader implications of the Very Large Telescope, which Winning strategy of the VLT’s success and to consider the received the green light from Council in next steps. 1987 and was built on Cerro Paranal in The VLT opened for business some five the Atacama desert between Antofagasta years after the Keck telescopes, but the and Taltal in Northern Chile. The 8.1m decision to take the time to build a fully Mission Gemini telescopes and the 8.3m Subaru integrated system, consisting of four telescope were constructed on a similar 8.2m telescopes and providing a dozen ESO’s mission is to enable scientific dis time scale, while the Large Binocular Tele foci for a carefully thoughtout comple coveries by constructing and operating scope and the Gran Telescopio Canarias ment of instruments together with four powerful observational facilities that are now starting operations. -
THE 1000 BRIGHTEST HIPASS GALAXIES: H I PROPERTIES B
The Astronomical Journal, 128:16–46, 2004 July A # 2004. The American Astronomical Society. All rights reserved. Printed in U.S.A. THE 1000 BRIGHTEST HIPASS GALAXIES: H i PROPERTIES B. S. Koribalski,1 L. Staveley-Smith,1 V. A. Kilborn,1, 2 S. D. Ryder,3 R. C. Kraan-Korteweg,4 E. V. Ryan-Weber,1, 5 R. D. Ekers,1 H. Jerjen,6 P. A. Henning,7 M. E. Putman,8 M. A. Zwaan,5, 9 W. J. G. de Blok,1,10 M. R. Calabretta,1 M. J. Disney,10 R. F. Minchin,10 R. Bhathal,11 P. J. Boyce,10 M. J. Drinkwater,12 K. C. Freeman,6 B. K. Gibson,2 A. J. Green,13 R. F. Haynes,1 S. Juraszek,13 M. J. Kesteven,1 P. M. Knezek,14 S. Mader,1 M. Marquarding,1 M. Meyer,5 J. R. Mould,15 T. Oosterloo,16 J. O’Brien,1,6 R. M. Price,7 E. M. Sadler,13 A. Schro¨der,17 I. M. Stewart,17 F. Stootman,11 M. Waugh,1, 5 B. E. Warren,1, 6 R. L. Webster,5 and A. E. Wright1 Received 2002 October 30; accepted 2004 April 7 ABSTRACT We present the HIPASS Bright Galaxy Catalog (BGC), which contains the 1000 H i brightest galaxies in the southern sky as obtained from the H i Parkes All-Sky Survey (HIPASS). The selection of the brightest sources is basedontheirHi peak flux density (Speak k116 mJy) as measured from the spatially integrated HIPASS spectrum. 7 ; 10 The derived H i masses range from 10 to 4 10 M . -
Giant H II Regions in the Merging System NGC 3256: Are They the Birthplaces of Globular Clusters?
CORE Metadata, citation and similar papers at core.ac.uk Provided by CERN Document Server Paper I: To be submitted to A.J. Giant H II regions in the merging system NGC 3256: Are they the birthplaces of globular clusters? J. English University of Manitoba K.C. Freeman Research School of Astronomy and Astrophysics, The Australian National University ABSTRACT CCD images and spectra of ionized hydrogen in the merging system NGC3256 were acquired as part of a kinematic study to investigate the formation of globular clusters (GC) during the interactions and mergers of disk galaxies. This paper focuses on the proposition by Kennicutt & Chu (1988) that giant H II regions, with an Hα luminosity > 1:5 1040 erg s 1, are birthplaces of young populous clusters (YPC’s ). × − Although NGC 3256 has relatively few (7) giant H II complexes, compared to some other interacting systems, these regions are comparable in total flux to about 85 30- Doradus-like H II regions (30-Dor GHR’s). The bluest, massive YPC’s (Zepf et al. 1999) are located in the vicinity of observed 30-Dor GHR’s, contributing to the notion that some fraction of 30-Dor GHR’s do cradle massive YPC’s, as 30 Dor harbors R136. If interactions induce the formation of 30-Dor GHR’s, the observed luminosities indi- cate that almost 900 30-Dor GHR’s would form in NGC 3256 throughout its merger epoch. In order for 30-Dor GHR’s to be considered GC progenitors, this number must be consistent with the specific frequencies of globular clusters estimated for elliptical galaxies formed via mergers of spirals (Ashman & Zepf 1993). -
Naming the Extrasolar Planets
Naming the extrasolar planets W. Lyra Max Planck Institute for Astronomy, K¨onigstuhl 17, 69177, Heidelberg, Germany [email protected] Abstract and OGLE-TR-182 b, which does not help educators convey the message that these planets are quite similar to Jupiter. Extrasolar planets are not named and are referred to only In stark contrast, the sentence“planet Apollo is a gas giant by their assigned scientific designation. The reason given like Jupiter” is heavily - yet invisibly - coated with Coper- by the IAU to not name the planets is that it is consid- nicanism. ered impractical as planets are expected to be common. I One reason given by the IAU for not considering naming advance some reasons as to why this logic is flawed, and sug- the extrasolar planets is that it is a task deemed impractical. gest names for the 403 extrasolar planet candidates known One source is quoted as having said “if planets are found to as of Oct 2009. The names follow a scheme of association occur very frequently in the Universe, a system of individual with the constellation that the host star pertains to, and names for planets might well rapidly be found equally im- therefore are mostly drawn from Roman-Greek mythology. practicable as it is for stars, as planet discoveries progress.” Other mythologies may also be used given that a suitable 1. This leads to a second argument. It is indeed impractical association is established. to name all stars. But some stars are named nonetheless. In fact, all other classes of astronomical bodies are named. -
The Nearby Eclipsing Stellar System Delta Velorum - IV
The nearby eclipsing stellar system delta Velorum - IV. Differential astrometry with VLT/NACO at the 100 microarcsecond level Pierre Kervella, Antoine Mérand, Monika Petr-Gotzens, Theo Pribulla, Frédéric Thévenin To cite this version: Pierre Kervella, Antoine Mérand, Monika Petr-Gotzens, Theo Pribulla, Frédéric Thévenin. The nearby eclipsing stellar system delta Velorum - IV. Differential astrometry with VLT/NACO at the 100 microarcsecond level. 2013. hal-00793521 HAL Id: hal-00793521 https://hal.archives-ouvertes.fr/hal-00793521 Preprint submitted on 22 Feb 2013 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. Astronomy & Astrophysics manuscript no. DelVel4-Astrom-v3r1 c ESO 2013 February 23, 2013 The nearby eclipsing stellar system δ Velorum IV. Differential astrometry with VLT/NACO at the 100 microarcsecond level ? P. Kervella1, A. Mérand2, M. G. Petr-Gotzens3, T. Pribulla4, and F. Thévenin5 1 LESIA, Observatoire de Paris, CNRS UMR 8109, UPMC, Université Paris Diderot, 5 place Jules Janssen, 92195 Meudon, France 2 European Southern Observatory, Alonso de Córdova 3107, Casilla 19001, Santiago 19, Chile 3 European Southern Observatory, Karl-Schwarzschild-Str. 2, D-85748 Garching, Germany 4 Astronomical Institute, Slovak Academy of Sciences, 059 60 Tatranská Lomnica, Slovakia 5 Université de Nice-Sophia Antipolis, Lab. -
Abstracts Connecting to the Boston University Network
20th Cambridge Workshop: Cool Stars, Stellar Systems, and the Sun July 29 - Aug 3, 2018 Boston / Cambridge, USA Abstracts Connecting to the Boston University Network 1. Select network ”BU Guest (unencrypted)” 2. Once connected, open a web browser and try to navigate to a website. You should be redirected to https://safeconnect.bu.edu:9443 for registration. If the page does not automatically redirect, go to bu.edu to be brought to the login page. 3. Enter the login information: Guest Username: CoolStars20 Password: CoolStars20 Click to accept the conditions then log in. ii Foreword Our story starts on January 31, 1980 when a small group of about 50 astronomers came to- gether, organized by Andrea Dupree, to discuss the results from the new high-energy satel- lites IUE and Einstein. Called “Cool Stars, Stellar Systems, and the Sun,” the meeting empha- sized the solar stellar connection and focused discussion on “several topics … in which the similarity is manifest: the structures of chromospheres and coronae, stellar activity, and the phenomena of mass loss,” according to the preface of the resulting, “Special Report of the Smithsonian Astrophysical Observatory.” We could easily have chosen the same topics for this meeting. Over the summer of 1980, the group met again in Bonas, France and then back in Cambridge in 1981. Nearly 40 years on, I am comfortable saying these workshops have evolved to be the premier conference series for cool star research. Cool Stars has been held largely biennially, alternating between North America and Europe. Over that time, the field of stellar astro- physics has been upended several times, first by results from Hubble, then ROSAT, then Keck and other large aperture ground-based adaptive optics telescopes. -
A Basic Requirement for Studying the Heavens Is Determining Where In
Abasic requirement for studying the heavens is determining where in the sky things are. To specify sky positions, astronomers have developed several coordinate systems. Each uses a coordinate grid projected on to the celestial sphere, in analogy to the geographic coordinate system used on the surface of the Earth. The coordinate systems differ only in their choice of the fundamental plane, which divides the sky into two equal hemispheres along a great circle (the fundamental plane of the geographic system is the Earth's equator) . Each coordinate system is named for its choice of fundamental plane. The equatorial coordinate system is probably the most widely used celestial coordinate system. It is also the one most closely related to the geographic coordinate system, because they use the same fun damental plane and the same poles. The projection of the Earth's equator onto the celestial sphere is called the celestial equator. Similarly, projecting the geographic poles on to the celest ial sphere defines the north and south celestial poles. However, there is an important difference between the equatorial and geographic coordinate systems: the geographic system is fixed to the Earth; it rotates as the Earth does . The equatorial system is fixed to the stars, so it appears to rotate across the sky with the stars, but of course it's really the Earth rotating under the fixed sky. The latitudinal (latitude-like) angle of the equatorial system is called declination (Dec for short) . It measures the angle of an object above or below the celestial equator. The longitud inal angle is called the right ascension (RA for short). -
Observing List Evening of 2011 Dec 25 at Boyden Observatory
Southern Skies Binocular list Observing List Evening of 2011 Dec 25 at Boyden Observatory Sunset 19:20, Twilight ends 20:49, Twilight begins 03:40, Sunrise 05:09, Moon rise 06:47, Moon set 20:00 Completely dark from 20:49 to 03:40. New Moon. All times local (GMT+2). Listing All Classes visible above 2 air mass and in complete darkness after 20:49 and before 03:40. Cls Primary ID Alternate ID Con Mag Size Distance RA 2000 Dec 2000 Begin Optimum End S.A. Ur. 2 PSA Difficulty Optimum EP Open Collinder 227 Melotte 101 Car 8.4 15.0' 6500 ly 10h42m12.0s -65°06'00" 01:32 03:31 03:54 25 210 40 challenging Glob NGC 2808 Car 6.2 14.0' 26000 ly 09h12m03.0s -64°51'48" 21:57 03:08 04:05 25 210 40 detectable Open IC 2602 Collinder 229 Car 1.6 100.0' 520 ly 10h42m58.0s -64°24'00" 23:20 03:31 04:07 25 210 40 obvious Open Collinder 246 Melotte 105 Car 9.4 5.0' 7200 ly 11h19m42.0s -63°29'00" 01:44 03:33 03:57 25 209 40 challenging Open IC 2714 Collinder 245 Car 8.2 14.0' 4000 ly 11h17m27.0s -62°44'00" 01:32 03:33 03:57 25 209 40 challenging Open NGC 2516 Collinder 172 Car 3.3 30.0' 1300 ly 07h58m04.0s -60°45'12" 20:38 01:56 04:10 24 200 30 obvious Open NGC 3114 Collinder 215 Car 4.5 35.0' 3000 ly 10h02m36.0s -60°07'12" 22:43 03:27 04:07 25 199 40 easy Neb NGC 3372 Eta Carinae Nebula Car 3.0 120.0' 10h45m06.0s -59°52'00" 23:26 03:32 04:07 25 199 38 easy Open NGC 3532 Collinder 238 Car 3.4 50.0' 1600 ly 11h05m39.0s -58°45'12" 23:47 03:33 04:08 25 198 38 easy Open NGC 3293 Collinder 224 Car 6.2 6.0' 7600 ly 10h35m51.0s -58°13'48" 23:18 03:32 04:08 25 199 -
CONFERENCE and REVIEW PUBLICATONS, and WHITE PAPERS: Reverse Chronological Harper, GM, 2013
CONFERENCE AND REVIEW PUBLICATONS, AND WHITE PAPERS: Reverse Chronological Harper, G. M., 2013, [Invited Review] Atmospheric structure and dynamics: the spatial and temporal domains, EAS Publications Series, Vol 60, 2013, pp.59-68 Farzone, M., Ryde, N., Harper, G. M., Lambert, J., Josselin, E., Richter, M. J., & Eriksson, K., 2013, What is the Origin of the Water Vapour Signatures in Red Giant Stars?, EAS Publications Series, Vol 60, pp.155-159 Carpenter, K. G., Ayres, T., Brown, A., Harper, G. M., & Wahlgren, G. M., 2012. The Amazing COS FUV (1320 - 1460A)˚ Spectrum of λ Vel (K4Ib-II), 16th Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun. Eds. C. M. Johns-Krull, M. K. Browning, and A. A. West. San Francisco: ASP Conf Ser., Vol. 448, p.1083 Harper, G. M., Brown, A., & Redfield, S., 2012, Constraints on the Surface Magnetic Field Structure of Aldebaran (αTauri, K5 III), 16th Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun. Eds. C. M. Johns-Krull, M. K. Browning, and A. A. West. San Francisco: ASP Conf Ser., Vol. 448, p.1145 O’Gorman, E. & Harper, G. M., 2012, What is Heating Arcturus’ Wind?, 16th Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun. Eds. C. M. Johns-Krull, M. K. Browning, and A. A. West. San Francisco: ASP Conf Ser., Vol. 448, p.691 van Belle, G. T., Aufdenberg, J., Boyajian, T., Harper G. M., Hummel, C., Pedretti, E., Baines, E., White, R., Ravi, V., & Ridgway, S., 2012, Fundamental Stellar Properties from Optical Interferometry, 16th Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun. -
List of Bright Nebulae Primary I.D. Alternate I.D. Nickname
List of Bright Nebulae Alternate Primary I.D. Nickname I.D. NGC 281 IC 1590 Pac Man Neb LBN 619 Sh 2-183 IC 59, IC 63 Sh2-285 Gamma Cas Nebula Sh 2-185 NGC 896 LBN 645 IC 1795, IC 1805 Melotte 15 Heart Nebula IC 848 Soul Nebula/Baby Nebula vdB14 BD+59 660 NGC 1333 Embryo Neb vdB15 BD+58 607 GK-N1901 MCG+7-8-22 Nova Persei 1901 DG 19 IC 348 LBN 758 vdB 20 Electra Neb. vdB21 BD+23 516 Maia Nebula vdB22 BD+23 522 Merope Neb. vdB23 BD+23 541 Alcyone Neb. IC 353 NGC 1499 California Nebula NGC 1491 Fossil Footprint Neb IC 360 LBN 786 NGC 1554-55 Hind’s Nebula -Struve’s Lost Nebula LBN 896 Sh 2-210 NGC 1579 Northern Trifid Nebula NGC 1624 G156.2+05.7 G160.9+02.6 IC 2118 Witch Head Nebula LBN 991 LBN 945 IC 405 Caldwell 31 Flaming Star Nebula NGC 1931 LBN 1001 NGC 1952 M 1 Crab Nebula Sh 2-264 Lambda Orionis N NGC 1973, 1975, Running Man Nebula 1977 NGC 1976, 1982 M 42, M 43 Orion Nebula NGC 1990 Epsilon Orionis Neb NGC 1999 Rubber Stamp Neb NGC 2070 Caldwell 103 Tarantula Nebula Sh2-240 Simeis 147 IC 425 IC 434 Horsehead Nebula (surrounds dark nebula) Sh 2-218 LBN 962 NGC 2023-24 Flame Nebula LBN 1010 NGC 2068, 2071 M 78 SH 2 276 Barnard’s Loop NGC 2149 NGC 2174 Monkey Head Nebula IC 2162 Ced 72 IC 443 LBN 844 Jellyfish Nebula Sh2-249 IC 2169 Ced 78 NGC Caldwell 49 Rosette Nebula 2237,38,39,2246 LBN 943 Sh 2-280 SNR205.6- G205.5+00.5 Monoceros Nebula 00.1 NGC 2261 Caldwell 46 Hubble’s Var. -
Gravity Distances of Planetary Nebulae Ii. Application to a Sample of Galactic Objects
GRAVITY DISTANCES OF PLANETARY NEBULAE II. APPLICATION TO A SAMPLE OF GALACTIC OBJECTS J. O. CAZETTA and W. J. MACIEL Instituto Astronômico e Geofísico da USP, Av. Miguel Stefano 4200, 04301-904 São Paulo SP, Brazil (Received 7 April 1999; accepted 28 October 1999) 1. Introduction The main results on the difficult problem of distance determination for planetary nebulae in the last few years derive from the application of trigonometric parallaxes (Harris et al. 1997), radio expansion method (Hajian et al., 1993, 1995) and Hippar- cos distances (Pottasch and Acker 1998, see also Terzian, 1993, 1997). However, these methods are necessarily restricted to a few objects, which remain a small fraction of the known population of galactic PN, estimated as around 1800 true and possible PN (Acker 1997). Therefore, there is still a need for the development of statistical methods, which may be applicable to a larger number of objects, even though at the cost of a lower accuracy. One such method is the so-called gravity distance method, proposed by Maciel and Cazetta (1997, hereafter referred to as Paper I). According to this method, an approximate range of progenitor masses can be attributed to the different PN types of the Peimbert classification scheme (Peimbert 1978, Peimbert and Torres- Peimbert 1983). Using theoretical initial mass-final mass relationships, the central star mass can be obtained. On the other hand, relations involving the surface gravity as a function of the central star temperature can also be derived for a given stellar mass, so that the luminosities of the central stars are obtained. -
Interstellar Reddening Towards Six Small Areas in Puppis-Vela⋆⋆⋆
A&A 543, A39 (2012) Astronomy DOI: 10.1051/0004-6361/201219007 & c ESO 2012 Astrophysics Interstellar reddening towards six small areas in Puppis-Vela, G. A. P. Franco Departamento de Física – ICEx – UFMG, Caixa Postal 702, 30.123-970 – Belo Horizonte – MG, Brazil e-mail: [email protected] Received 9 February 2012 / Accepted 1 May 2012 ABSTRACT Context. The line-of-sight towards Puppis-Vela contains some of the most interesting and elusive objects in the solar neighbourhood, including the Gum nebula, the IRAS Vela shell, the Vela SNR, and dozens of cometary globules. Aims. We investigate the distribution of the interstellar dust towards six small volumes of the sky in the region of the Gum nebula. Methods. New high-quality four-colour uvby and Hβ Strömgren photometry obtained for 352 stars in six selected areas of Kapteyn and complemented with data obtained in a previous investigation for two of these areas, were used to estimate the colour excess and distance to these objects. The obtained colour excess versus distance diagrams, complemented with other information, when available, were analysed in order to infer the properties of the interstellar medium permeating the observed volumes. Results. On the basis of the overall standard deviation in the photometric measurements, we estimate that colour excesses and distances are determined with an accuracy of 0m. 010 and better than 30%, respectively, for a sample of 520 stars. A comparison with 37 stars in common with the new Hipparcos catalogue attests to the high quality of the photometric distance determination. The obtained colour excess versus distance diagrams testify to the low density volume towards the observed lines-of-sight.