STATISTICS and PROPERTIES of Hii REGIONS in a SAMPLE OF
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A Multi-Transition HCN and HCO+ Study of 12 Nearby Active Galaxies
Draft version October 31, 2018 Preprint typeset using LATEX style emulateapj v. 08/22/09 A MULTI-TRANSITION HCN AND HCO+ STUDY OF 12 NEARBY ACTIVE GALAXIES: AGN VERSUS SB ENVIRONMENTS M. Krips1, R. Neri2, S. Garc´ıa-Burillo3, S. Mart´ın1, F. Combes4, J. Gracia-Carpio´ 3, and A. Eckart5 Draft version October 31, 2018 ABSTRACT Recent studies have indicated that the HCN-to-CO(J=1–0) and HCO+-to-HCN(J=1–0) ratios are significantly different between galaxies with AGN (active galactic nucleus) and SB (starburst) sig- natures. In order to study the molecular gas properties in active galaxies and search for differences between AGN and SB environments, we observed the HCN(J=1–0), (J=2–1), (J=3–2), HCO+(J=1– 0) and HCO+(J=3–2) emission with the IRAM 30m in the centre of 12 nearby active galaxies which either exhibit nuclear SB and/or AGN signatures. Consistent with previous results, we find a sig- nificant difference of the HCN(J=2–1)-to-HCN(J=1–0), HCN(J=3–2)-to-HCN(J=1–0), HCO+(J=3– 2)-to-HCO+(J=1–0) and HCO+-to-HCN intensity ratios between the sources dominated by an AGN and those with an additional or pure central SB: the HCN, HCO+ and HCO+-to-HCN intensity ra- tios tend to be higher in the galaxies of our sample with a central SB as opposed to the pure AGN cases which show rather low intensity ratios. Based on an LVG analysis of these data, i.e., assuming purely collisional excitation, the (average) molecular gas densities in the SB dominated sources of our sample seem to be systematically higher than in the AGN sources. -
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Near-Infrared Photometry of Isolated Spirals with and Without an AGN
ASTRONOMY & ASTROPHYSICS NOVEMBER II 1999,PAGE1 SUPPLEMENT SERIES Astron. Astrophys. Suppl. Ser. 140, 1–14 (1999) Near-infrared photometry of isolated spirals with and without an AGN I. The data ?;?? I. M´arquez1,2, F. Durret2,3, R.M. Gonz´alez Delgado1, I. Marrero1,J.Masegosa1,J.Maza4,M.Moles5,E.P´erez1, and M. Roth6 1 Instituto de Astrof´ısica de Andaluc´ıa (CSIC), Apartado 3004, E-18080 Granada, Spain 2 Institut d’Astrophysique de Paris, CNRS, 98bis Bd. Arago, F-75014 Paris, France 3 DAEC, Observatoire de Paris, Universit´e Paris VII, CNRS (UA 173), F-92195 Meudon Cedex, France 4 Departamento de Astronom´ıa, Universidad de Chile, Casilla 36D, Santiago, Chile 5 Instituto de Matem´aticas y F´ısica Fundamental (CSIC), Madrid, Spain and Observatorio Astron´omico Nacional, Madrid, Spain. Presently on sabbatical leave at Queen Mary & Westfield College, London, UK 6 Observatories of the Carnegie Institution of Washington, 813 Barbara Street, Pasadena, CA 91101, U.S.A. Received May 5; accepted August 27, 1999 Abstract. We present infrared imaging data in the J and ences between active and non active galaxies in the prop- K0 bands obtained for 18 active spiral galaxies, together erties of their central regions that could be connected with with 11 non active galaxies taken as a control sample. All the onset of nuclear activity. of them were chosen to satisfy well defined isolation crite- ria so that the observed properties are not related to grav- Key words: galaxies: active — galaxies: fundamental itational interaction. For each object we give: the image in parameters — galaxies: photometry — infrared: galaxies the K0 band, the sharp-divided image (obtained by divid- ing the observed image by a filtered one), the difference image (obtained by subtracting a model to the observed one), the color J − K0 image, the ellipticity and position angle profiles, the surface brightness profiles in J and K0, 1. -
Dark Matter Deprivation in the Field Elliptical Galaxy NGC 7507⋆
A&A 574, A93 (2015) Astronomy DOI: 10.1051/0004-6361/201424074 & c ESO 2015 Astrophysics Dark matter deprivation in the field elliptical galaxy NGC 7507 Richard R. Lane1, Ricardo Salinas2, and Tom Richtler1 1 Departamento de Astronomía Universidad de Concepción, Casilla 160 C, Concepción, Chile e-mail: [email protected] 2 Department of Physics and Astronomy, Michigan State University, East Lansing, MI 48824, USA Received 25 April 2014 / Accepted 10 December 2014 ABSTRACT Context. Previous studies have shown that the kinematics of the field elliptical galaxy NGC 7507 do not necessarily require dark matter. This is troubling because, in the context of ΛCDM cosmologies, all galaxies should have a large dark matter component. Aims. Our aims are to determine the rotation and velocity dispersion profile out to larger radii than do previous studies, and, therefore, more accurately estimate of the dark matter content of the galaxy. Methods. We use penalised pixel-fitting software to extract velocities and velocity dispersions from GMOS slit mask spectra. Using Jeans and MONDian modelling, we then produce models with the goal of fitting the velocity dispersion data. Results. NGC 7507 has a two-component stellar halo, with the outer halo counter rotating with respect to the inner halo, with a kinematic boundary at a radius of ∼110 (∼12.4 kpc). The velocity dispersion profile exhibits an increase at ∼70 (∼7.9 kpc), reminiscent of several other elliptical galaxies. Our best fit models are those under mild anisotropy, which include ∼100 times less dark matter than predicted by ΛCDM, although mildly anisotropic models that are completely dark matter free fit the measured dynamics almost equally well. -
7.5 X 11.5.Threelines.P65
Cambridge University Press 978-0-521-19267-5 - Observing and Cataloguing Nebulae and Star Clusters: From Herschel to Dreyer’s New General Catalogue Wolfgang Steinicke Index More information Name index The dates of birth and death, if available, for all 545 people (astronomers, telescope makers etc.) listed here are given. The data are mainly taken from the standard work Biographischer Index der Astronomie (Dick, Brüggenthies 2005). Some information has been added by the author (this especially concerns living twentieth-century astronomers). Members of the families of Dreyer, Lord Rosse and other astronomers (as mentioned in the text) are not listed. For obituaries see the references; compare also the compilations presented by Newcomb–Engelmann (Kempf 1911), Mädler (1873), Bode (1813) and Rudolf Wolf (1890). Markings: bold = portrait; underline = short biography. Abbe, Cleveland (1838–1916), 222–23, As-Sufi, Abd-al-Rahman (903–986), 164, 183, 229, 256, 271, 295, 338–42, 466 15–16, 167, 441–42, 446, 449–50, 455, 344, 346, 348, 360, 364, 367, 369, 393, Abell, George Ogden (1927–1983), 47, 475, 516 395, 395, 396–404, 406, 410, 415, 248 Austin, Edward P. (1843–1906), 6, 82, 423–24, 436, 441, 446, 448, 450, 455, Abbott, Francis Preserved (1799–1883), 335, 337, 446, 450 458–59, 461–63, 470, 477, 481, 483, 517–19 Auwers, Georg Friedrich Julius Arthur v. 505–11, 513–14, 517, 520, 526, 533, Abney, William (1843–1920), 360 (1838–1915), 7, 10, 12, 14–15, 26–27, 540–42, 548–61 Adams, John Couch (1819–1892), 122, 47, 50–51, 61, 65, 68–69, 88, 92–93, -
190 Index of Names
Index of names Ancora Leonis 389 NGC 3664, Arp 005 Andriscus Centauri 879 IC 3290 Anemodes Ceti 85 NGC 0864 Name CMG Identification Angelica Canum Venaticorum 659 NGC 5377 Accola Leonis 367 NGC 3489 Angulatus Ursae Majoris 247 NGC 2654 Acer Leonis 411 NGC 3832 Angulosus Virginis 450 NGC 4123, Mrk 1466 Acritobrachius Camelopardalis 833 IC 0356, Arp 213 Angusticlavia Ceti 102 NGC 1032 Actenista Apodis 891 IC 4633 Anomalus Piscis 804 NGC 7603, Arp 092, Mrk 0530 Actuosus Arietis 95 NGC 0972 Ansatus Antliae 303 NGC 3084 Aculeatus Canum Venaticorum 460 NGC 4183 Antarctica Mensae 865 IC 2051 Aculeus Piscium 9 NGC 0100 Antenna Australis Corvi 437 NGC 4039, Caldwell 61, Antennae, Arp 244 Acutifolium Canum Venaticorum 650 NGC 5297 Antenna Borealis Corvi 436 NGC 4038, Caldwell 60, Antennae, Arp 244 Adelus Ursae Majoris 668 NGC 5473 Anthemodes Cassiopeiae 34 NGC 0278 Adversus Comae Berenices 484 NGC 4298 Anticampe Centauri 550 NGC 4622 Aeluropus Lyncis 231 NGC 2445, Arp 143 Antirrhopus Virginis 532 NGC 4550 Aeola Canum Venaticorum 469 NGC 4220 Anulifera Carinae 226 NGC 2381 Aequanimus Draconis 705 NGC 5905 Anulus Grahamianus Volantis 955 ESO 034-IG011, AM0644-741, Graham's Ring Aequilibrata Eridani 122 NGC 1172 Aphenges Virginis 654 NGC 5334, IC 4338 Affinis Canum Venaticorum 449 NGC 4111 Apostrophus Fornac 159 NGC 1406 Agiton Aquarii 812 NGC 7721 Aquilops Gruis 911 IC 5267 Aglaea Comae Berenices 489 NGC 4314 Araneosus Camelopardalis 223 NGC 2336 Agrius Virginis 975 MCG -01-30-033, Arp 248, Wild's Triplet Aratrum Leonis 323 NGC 3239, Arp 263 Ahenea -
Making a Sky Atlas
Appendix A Making a Sky Atlas Although a number of very advanced sky atlases are now available in print, none is likely to be ideal for any given task. Published atlases will probably have too few or too many guide stars, too few or too many deep-sky objects plotted in them, wrong- size charts, etc. I found that with MegaStar I could design and make, specifically for my survey, a “just right” personalized atlas. My atlas consists of 108 charts, each about twenty square degrees in size, with guide stars down to magnitude 8.9. I used only the northernmost 78 charts, since I observed the sky only down to –35°. On the charts I plotted only the objects I wanted to observe. In addition I made enlargements of small, overcrowded areas (“quad charts”) as well as separate large-scale charts for the Virgo Galaxy Cluster, the latter with guide stars down to magnitude 11.4. I put the charts in plastic sheet protectors in a three-ring binder, taking them out and plac- ing them on my telescope mount’s clipboard as needed. To find an object I would use the 35 mm finder (except in the Virgo Cluster, where I used the 60 mm as the finder) to point the ensemble of telescopes at the indicated spot among the guide stars. If the object was not seen in the 35 mm, as it usually was not, I would then look in the larger telescopes. If the object was not immediately visible even in the primary telescope – a not uncommon occur- rence due to inexact initial pointing – I would then scan around for it. -
Optical Spectroscopy of the Central Regions of Bright Barred Spiral
Optical Spectroscopy of the Central oeste. Las densidades electr´onicas se han estimado de Regions of Bright Barred Spiral los cocientes de l´ıneas de azufre [SII]. Galaxies Optical red spectra of a set of 18 bright barred spiral galaxies are presented. The study is aimed at J.A. Garc´ıa-Barreto1, H. Aceves2, O. Kuhn3, G. determining the local kinematics, and physical condi- Canalizo4, R. Carrillo1 tions of ionized gas in the compact nucleus (inside a and diameter of 5′′) and in the circumnuclear regions (in- ′′ J. Franco1 side a diameter of 20 ). Only 8 galaxies showed bright emission from their east and west side of the nucleus. Abstract The spectrum of each region was analized separately. In other 10 galaxies the line emission was so weak Se presentan espectros ´opticos en la banda roja de that we were only able to obtain an average spectrum 18 galaxias espirales con barra. El estudio se enfoca of the central emission. No emission was detected in a la determinaci´on de la cinem´atica local y condi- the remaining 8 galaxies. An estimate of the dynami- ciones del gas ionizado en el n´ucleo compacto (dentro cal mass is presented based on the observed velocities de un diametro de 5′′) y en las regiones circunnucle- in the circumnuclear regions. In NGC 4314 and NGC ares (dentro de un diametro de 20′′). S´olo 8 galax- 6951, that show Hα emission distributed in circumnu- ias presentan emision brillante al Este y Oeste del clear ring structures, we determine the [NII]/Hα and n´ucleo compacto. -
The Eldorado Star Party 2013 Binocular and Telescope Observing
The Eldorado Star Party 2013 Binocular and Telescope Observing Clubs by Bill Flanagan Houston Astronomical Society (in collaboration with Blackie Bolduc and Brad Walter) Purpose and Rules Welcome to the Annual ESP Binocular and Telescope Clubs! The main purpose of these clubs is to give you an opportunity to observe some of the showpiece objects of the fall season under the pristine skies of Southwest Texas. In addition, we have included a few objects in the observing lists that may challenge you to observe some fainter and more obscure objects that present themselves at their very best under the dark skies of ESP. The rules are simple. Just observe the required number of objects listed for each program while you are at the Eldorado Star Party to receive a club badge. Binocular Club The binocular club program is a list consisting of 24 objects called “Great Balls of Fire”. All of the objects in this list are globular clusters and should be observable from the Eldorado Star Party with a good pair of binoculars. You need to observe only 15 out of the 24 objects to qualify for the Binocular Observing Club badge. Cheat sheets for finding these objects are available on the ESP website. Telescope Club The telescope program is a list consisting of 26 objects, all located in the constellations of Cepheus and Cassiopeia. The title of this program is “Ransack the Palace,” and of course the goal of this program is to bag the most precious and beautiful jewels from the palace of King Cepheus and Queen Cassiopeia. -
Radio Observations of the Circumnuclear Ring in NGC 6951
A&A 383, 98–103 (2002) Astronomy DOI: 10.1051/0004-6361:20011710 & c ESO 2002 Astrophysics Radio observations of the circumnuclear ring in NGC 6951 D. J. Saikia1,2,3, B. Phookun4,A.Pedlar2,5, and K. Kohno6,7 1 Department of Physics, Queen’s University, Kingston, Ontario, K7L 3N6, Canada 2 Jodrell Bank Observatory, University of Manchester, Macclesfield, Cheshire SK11 9DL, UK 3 National Centre for Radio Astrophysics, Tata Institute of Fundamental Research, Post Bag No. 3, Ganeshkhind, Pune 411 007, India 4 St. Stephen’s College, University of Delhi, Delhi 110 007, India 5 Onsala Space Observatory, 43992 Onsala, Sweden 6 Nobeyama Radio Observatory, Minamimaki, Minamisaku, Nagano 384-1305, Japan 7 Institute of Astronomy, University of Tokyo, Osawa, Mitaka, Tokyo 181-0015, Japan Received 26 September 2001 / Accepted 3 December 2001 Abstract. We present sensitive, high-resolution radio observations of the circumnuclear region of the barred spiral galaxy NGC 6951. These observations reveal a ring of radio emission with many discrete components and a marginally resolved nuclear component. We compare the radio ring with observations at other wavelengths, and discuss the nature of the compact radio components. Key words. galaxies: active – galaxies: individual: NGC 6951 – galaxies: nuclei – galaxies: spiral – radio continuum: galaxies 1. Introduction Combes & Gerin 1985; Athanassoula 1992; Byrd et al. 1994; Piner et al. 1995). The dense gas which accumu- The dynamics and relationships between gas inflow pro- lates in an ILR ring leads to a high star-formation rate cesses, circumnuclear star formation and the presence of either due to collisions of the molecular clouds (Combes an active nucleus are important, since they might pro- & Gerin 1985), or gravitational collapse in the ring when vide valuable leads towards understanding the transport the density reaches a critical value (Elmegreen 1994). -
Atlante Grafico Delle Galassie
ASTRONOMIA Il mondo delle galassie, da Kant a skylive.it. LA RIVISTA DELL’UNIONE ASTROFILI ITALIANI Questo è un numero speciale. Viene qui presentato, in edizione ampliata, quan- [email protected] to fu pubblicato per opera degli Autori nove anni fa, ma in modo frammentario n. 1 gennaio - febbraio 2007 e comunque oggigiorno di assai difficile reperimento. Praticamente tutte le galassie fino alla 13ª magnitudine trovano posto in questo atlante di più di Proprietà ed editore Unione Astrofili Italiani 1400 oggetti. La lettura dell’Atlante delle Galassie deve essere fatto nella sua Direttore responsabile prospettiva storica. Nella lunga introduzione del Prof. Vincenzo Croce il testo Franco Foresta Martin Comitato di redazione e le fotografie rimandano a 200 anni di studio e di osservazione del mondo Consiglio Direttivo UAI delle galassie. In queste pagine si ripercorre il lungo e paziente cammino ini- Coordinatore Editoriale ziato con i modelli di Herschel fino ad arrivare a quelli di Shapley della Via Giorgio Bianciardi Lattea, con l’apertura al mondo multiforme delle altre galassie, iconografate Impaginazione e stampa dai disegni di Lassell fino ad arrivare alle fotografie ottenute dai colossi della Impaginazione Grafica SMAA srl - Stampa Tipolitografia Editoria DBS s.n.c., 32030 metà del ‘900, Mount Wilson e Palomar. Vecchie fotografie in bianco e nero Rasai di Seren del Grappa (BL) che permettono al lettore di ripercorrere l’alba della conoscenza di questo Servizio arretrati primo abbozzo di un Universo sempre più sconfinato e composito. Al mondo Una copia Euro 5.00 professionale si associò quanto prima il mondo amatoriale. Chi non è troppo Almanacco Euro 8.00 giovane ricorderà le immagini ottenute dal cielo sopra Bologna da Sassi, Vac- Versare l’importo come spiegato qui sotto specificando la causale. -
Small Wonders: Cepheus a Monthly Sky Guide for the Beginning to Intermediate Amateur Astronomer Tom Trusock 11-Sep-2005
Small Wonders: Cepheus A monthly sky guide for the beginning to intermediate amateur astronomer Tom Trusock 11-Sep-2005 Figure 1. W idefield map 2/11 Small Wonders: Cepheus Target List Object Type Size Mag RA Dec µ (mu) Cephei (Garnet star) Star 4.2 21h 43m 42.2s +58° 48' 27" KR 60 Star 9.6 22h 28m 14.4s +57° 43' 37" IC 1396 Reflection Nebula 90.0' 21h 39m 17.8s +57° 31' 38" NGC 40 Planetary Nebula 1.2' 12.3 00h 13m 21.7s +72° 33' 12" NGC 188 Open Cluster 15.0' 8.1 00h 48m 10.8s +85° 17' 04" NGC 6939 Open Cluster 10.0' 7.8 20h 31m 38.0s +60° 41' 00" NGC 6951 Galaxy 3.9'x3.2' 11 20h 37m 19.6s +66° 07' 39" NGC 7023 Bright Nebula 10.0'x8.0' 7.1 21h 01m 41.3s +68° 11' 36" NGC 7354 Planetary Nebula 36" 12.2 22h 40m 34.1s +61° 18' 59" NGC 7510 Open Cluster 7.0' 7.9 23h 11m 19.7s +60° 36' 07" Challenge Objects Object Type Size Mag RA Dec Sh2-155 Bright Nebula 50.0'x30.0' 22h 57m 02.9s +62° 38' 51" Cepheus ur celestial personality for the month – Cepheus – is the son of Belus, King of Eqypt. Cepheus became King of Ethiopia and entered celestial mythology as both the husband of O Cassiopiea and the father of Andromeda. According to one legend, both Cepheus and Cassiopiea are killed at Andromeda‘s wedding to Peresus. Poseidon then places both in the night sky to immortalize them.