THE Paα LUMINOSITY FUNCTION of HII REGIONS in NEARBY
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The Newsletter of the Barnard-Seyfert Astronomical Society
March The ECLIPSE 2018 The Newsletter of the Barnard-Seyfert Astronomical Society From the President Next Membership Meeting: Greetings, March 21, 2018, 7:30 pm February 2018 was no friend of BSAS weather wise. Te short Cumberland Valley month of February was not short on rain. We saw 18 or 19 Girl Scout Council Building days with measurable participation. Average monthly rainfall 4522 Granny White Pike in February for Nashville is 3.7 inches. We had just under 11 inches. When it wasn’t raining it was cloudy and windy. Topic: Equipment Tune-up Details on page 6. We had enough bad weather to frustrate almost all attempts to view the winter stars and deep sky objects we believe are still up there. Our public star party at Edwin Warner Park was washed out, as was the private star party on the Natchez In this Issue: Trace at Water Valley Overlook. May we turn the page on that trend? Observing Highlights 2 Tanks to Terry Reeves for his informative and helpful From A Certain Point of View presentation, All About A Messier Marathon, which he gave reviewed by Robin Byrne 3 at this month’s member meeting. We will have a chance to put that information into practice on Saturday, March 17th Deep Sky Daze when BSAS holds a Messier Marathon at Mark Manner’s by Mike Benson 4 Spot Observatory. Just in case, we are planning April 14th as Board Meeting Minutes 8 a backup date. We have that date reserved for a private star February 7, 2018 party at Water Valley Overlook. -
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). -
Lemmings. I. the Emerlin Legacy Survey of Nearby Galaxies. 1.5-Ghz Parsec-Scale Radio Structures and Cores
MNRAS 000,1{44 (2018) Preprint 8 February 2018 Compiled using MNRAS LATEX style file v3.0 LeMMINGs. I. The eMERLIN legacy survey of nearby galaxies. 1.5-GHz parsec-scale radio structures and cores R. D. Baldi1?, D. R. A. Williams1, I. M. McHardy1, R. J. Beswick2, M. K. Argo2;3, B. T. Dullo4, J. H. Knapen5;6, E. Brinks7, T. W. B. Muxlow2, S. Aalto8, A. Alberdi9, G. J. Bendo2;10, S. Corbel11;12, R. Evans13, D. M. Fenech14, D. A. Green15, H.-R. Kl¨ockner16, E. K¨ording17, P. Kharb18, T. J. Maccarone19, I. Mart´ı-Vidal8, C. G. Mundell20, F. Panessa21, A. B. Peck22, M. A. P´erez-Torres9, D. J. Saikia18, P. Saikia17;23, F. Shankar1, R. E. Spencer2, I. R. Stevens24, P. Uttley25 and J. Westcott7 1 School of Physics and Astronomy, University of Southampton, Southampton, SO17 1BJ, UK 2 Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, The University of Manchester, Manchester, M13 9PL, UK 3 Jeremiah Horrocks Institute, University of Central Lancashire, Preston PR1 2HE, UK 4 Departamento de Astrofisica y Ciencias de la Atmosfera, Universidad Complutense de Madrid, E-28040 Madrid, Spain 5 Instituto de Astrofisica de Canarias, Via Lactea S/N, E-38205, La Laguna, Tenerife, Spain 6 Departamento de Astrofisica, Universidad de La Laguna, E-38206, La Laguna, Tenerife, Spain 7 Centre for Astrophysics Research, University of Hertfordshire, College Lane, Hatfield, AL10 9AB, UK 8 Department of Space, Earth and Environment, Chalmers University of Technology, Onsala Space Observatory, 43992 Onsala, Sweden 9 Instituto de Astrofisica de Andaluc´ıa(IAA, CSIC); Glorieta de la Astronom´ıa s/n, 18008-Granada, Spain 10 ALMA Regional Centre Node, UK 11 Laboratoire AIM (CEA/IRFU - CNRS/INSU - Universit´eParis Diderot), CEA DSM/IRFU/SAp, F-91191 Gif-sur-Yvette, France 12 Station de Radioastronomie de Nan¸cay, Observatoire de Paris, PSL Research University, CNRS, Univ. -
Corrugated Velocity Patterns in the Spiral Galaxies: NGC 278, NGC 1058, NGC 2500 & UGC 3574
Mem. S.A.It. Suppl. Vol. 25, 86 Memorie della c SAIt 2013 Supplementi Corrugated velocity patterns in the spiral galaxies: NGC 278, NGC 1058, NGC 2500 & UGC 3574 M. C. Sanchez´ Gil1, E. J. Alfaro2, and E. Perez´ 2 1 Universidad de Cadiz,´ Facultad de Ciencias Poligono Rio San Pedro 11510 - Puerto Real, Spain, e-mail: [email protected] 2 Instituto de Astrof´ısica de Andaluc´ıa (CSIC), E18008, Granada, Spain Abstract. In this work we address the study of the detection in Hα of a radial corruga- tion in the vertical velocity field in a sample of four nearly face-on, spiral galaxies. The geometry of the problem is a main criterion in the selection of the sample as well as of the azimuthal angle of the slits. These spatial corrugations must be equally associated with wavy vertical motions in the galactic plane with a strong large-scale consistency. Evidence of these kinematic waves were first detected in the analysis of the rotation curves of spiral galaxies (eg Vaucoleurs & de Vaucaleurs 1963, Pismis 1965), but it was not until 2001 that Alfaro et al. analyzed in more detail the velocity corrugations in NGC 5427 and a possi- ble physical mechanism for their origin. The aim of this study is to analyze the corrugated velocity pattern in terms of the star formation processes. We describe the geometry of the problem and establish its fundamental relationships. Key words. Techniques: spectroscopic–Galaxies: kinematics and dynamics - spiral - struc- ture 1. Introduction & Delgado 1992) and both in the azimuthal direction along different spiral arms (Spicker The disks of spiral galaxies are highly struc- & Feitzinger 1986), as in the radial, in differ- tured. -
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. -
WHAT 'S UP? November 2016
WHAT 'S UP? November 2016 Temecula Valley Astronomers http://www.temeculavalleyastronomers.com METEOR SHOWERS - South Taurids Occurs September 25 – November 25 , Peak 11/4-5 - North Taurids Occurs from October 12 – December 2, Peal 11/11-12 - Leonids Occurs from Nov 6 – Nov 23, Peak on 11/16 -17 - zenith hourly rate 15/hr - Moon phase almost (81%) full (moonrise 20:16) - Geminids Occurs from Dec 7 – Dec 17, Peak on 12/13 -14 - zenith hourly rate 120/hr - Moon phase full (moon rise @16:56) “SUPER MOONS” Two more this year! -November 14 – “Beaver” moon - 6am EST, the centers of the Earth and Moon will be just 221,275 miles apart. Closest since 1976, and won’t be as close again until 2020. -December 14 – “Full Cold Moon” November 7 CASSIOPEIA Prominent northern constellation, named after Queen Cassiopeia One of the original 48 constellations plotted by Ptolemy, and remains one of the 88 today One of the most recognizable due to the “W” shape of the 5 brightest stars Located right in the center of the Milky Way, featuring over a dozen bright open clusters, double and variable stars, 4 nebula, and 3 galaxies In the most northern latitudes, it is circumpolar, so visible year round. STARS, STARS, STARS! ALGOL (β Per) (VARIABLE STAR) CASSIOPEIA OBJECTS Clusters Nebula NGC 869 and NGC 884 - The Double Cluster ** NGC 281 (Pacman Nebula) M34 - Spiral Cluster NGC 7635 (The Bubble Nebula) M52 ** IC 1805 (Heart Nebula) M103 - open cluster ** IC 1848 (Soul Nebula) Stock 2 ** IC 59 and IC 63 (challenging) NGC 129 ** NGC 225 (Sailboat Cluster) ** Galaxies -
Nuclear Activity in Circumnuclear Ring Galaxies
International Journal of Astronomy and Astrophysics, 2016, 6, 219-235 Published Online September 2016 in SciRes. http://www.scirp.org/journal/ijaa http://dx.doi.org/10.4236/ijaa.2016.63018 Nuclear Activity in Circumnuclear Ring Galaxies María P. Agüero1, Rubén J. Díaz2,3, Horacio Dottori4 1Observatorio Astronómico de Córdoba, UNCand CONICET, Córdoba, Argentina 2ICATE, CONICET, San Juan, Argentina 3Gemini Observatory, La Serena, Chile 4Instituto de Física, UFRGS, Porto Alegre, Brazil Received 23 May 2016; accepted 26 July 2016; published 29 July 2016 Copyright © 2016 by authors and Scientific Research Publishing Inc. This work is licensed under the Creative Commons Attribution International License (CC BY). http://creativecommons.org/licenses/by/4.0/ Abstract We have analyzed the frequency and properties of the nuclear activity in a sample of galaxies with circumnuclear rings and spirals (CNRs), compiled from published data. From the properties of this sample a typical circumnuclear ring can be characterized as having a median radius of 0.7 kpc (mean 0.8 kpc, rms 0.4 kpc), located at a spiral Sa/Sb galaxy (75% of the hosts), with a bar (44% weak, 37% strong bars). The sample includes 73 emission line rings, 12 dust rings and 9 stellar rings. The sample was compared with a carefully matched control sample of galaxies with very similar global properties but without detected circumnuclear rings. We discuss the relevance of the results in regard to the AGN feeding processes and present the following results: 1) bright companion galaxies seem -
GHASP: an Halpha Kinematic Survey of Spiral and Irregular Galaxies - IV
GHASP: an Halpha kinematic survey of spiral and irregular galaxies - IV. 44 new velocity fields. Extension, shape and asymmetry of Halpha rotation curves P. Amram, C. Balkowski, J. Boulesteix, J.L. Gach, O. Garrido, M. Marcelin To cite this version: P. Amram, C. Balkowski, J. Boulesteix, J.L. Gach, O. Garrido, et al.. GHASP: an Halpha kinematic survey of spiral and irregular galaxies - IV. 44 new velocity fields. Extension, shape and asymmetry of Halpha rotation curves. Monthly Notices of the Royal Astronomical Society, Oxford University Press (OUP): Policy P - Oxford Open Option A, 2005, 362, pp.127. 10.1111/j.1365-2966.2005.09274.x. hal-00017198 HAL Id: hal-00017198 https://hal.archives-ouvertes.fr/hal-00017198 Submitted on 13 Dec 2020 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. Mon. Not. R. Astron. Soc. 362, 127–166 (2005) doi:10.1111/j.1365-2966.2005.09274.x GHASP: an Hα kinematic survey of spiral and irregular galaxies – IV. 44 new velocity fields. Extension, shape and asymmetry of Hα rotation curves , O. Garrido,1 2 M. Marcelin,2 P. Amram,2 C. Balkowski,1 J. -
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. -
Ngc Catalogue Ngc Catalogue
NGC CATALOGUE NGC CATALOGUE 1 NGC CATALOGUE Object # Common Name Type Constellation Magnitude RA Dec NGC 1 - Galaxy Pegasus 12.9 00:07:16 27:42:32 NGC 2 - Galaxy Pegasus 14.2 00:07:17 27:40:43 NGC 3 - Galaxy Pisces 13.3 00:07:17 08:18:05 NGC 4 - Galaxy Pisces 15.8 00:07:24 08:22:26 NGC 5 - Galaxy Andromeda 13.3 00:07:49 35:21:46 NGC 6 NGC 20 Galaxy Andromeda 13.1 00:09:33 33:18:32 NGC 7 - Galaxy Sculptor 13.9 00:08:21 -29:54:59 NGC 8 - Double Star Pegasus - 00:08:45 23:50:19 NGC 9 - Galaxy Pegasus 13.5 00:08:54 23:49:04 NGC 10 - Galaxy Sculptor 12.5 00:08:34 -33:51:28 NGC 11 - Galaxy Andromeda 13.7 00:08:42 37:26:53 NGC 12 - Galaxy Pisces 13.1 00:08:45 04:36:44 NGC 13 - Galaxy Andromeda 13.2 00:08:48 33:25:59 NGC 14 - Galaxy Pegasus 12.1 00:08:46 15:48:57 NGC 15 - Galaxy Pegasus 13.8 00:09:02 21:37:30 NGC 16 - Galaxy Pegasus 12.0 00:09:04 27:43:48 NGC 17 NGC 34 Galaxy Cetus 14.4 00:11:07 -12:06:28 NGC 18 - Double Star Pegasus - 00:09:23 27:43:56 NGC 19 - Galaxy Andromeda 13.3 00:10:41 32:58:58 NGC 20 See NGC 6 Galaxy Andromeda 13.1 00:09:33 33:18:32 NGC 21 NGC 29 Galaxy Andromeda 12.7 00:10:47 33:21:07 NGC 22 - Galaxy Pegasus 13.6 00:09:48 27:49:58 NGC 23 - Galaxy Pegasus 12.0 00:09:53 25:55:26 NGC 24 - Galaxy Sculptor 11.6 00:09:56 -24:57:52 NGC 25 - Galaxy Phoenix 13.0 00:09:59 -57:01:13 NGC 26 - Galaxy Pegasus 12.9 00:10:26 25:49:56 NGC 27 - Galaxy Andromeda 13.5 00:10:33 28:59:49 NGC 28 - Galaxy Phoenix 13.8 00:10:25 -56:59:20 NGC 29 See NGC 21 Galaxy Andromeda 12.7 00:10:47 33:21:07 NGC 30 - Double Star Pegasus - 00:10:51 21:58:39 -
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. -
Using Hubble Space Telescope Imaging of Nuclear Dust
To be published in the Astronomical Journal, June 1999 Using Hubble Space Telescope Imaging of Nuclear Dust Morphology to Rule Out Bars Fueling Seyfert Nuclei1 Michael W. Regan2,3 Carnegie Institution of Washington, Department of Terrestrial Magnetism, 5241 Broad Branch Road, Washington, DC 20015 John S. Mulchaey4 The Observatories of the Carnegie Institution of Washington, 813 Santa Barbara Street, Pasadena, CA 91101 ABSTRACT If AGN are powered by the accretion of matter onto massive black holes, how does the gas in the host galaxy lose the required angular momentum to approach the black hole? Gas easily transfers angular momentum to stars in strong bars, making them likely candidates. Although ground-based searches for bars in active galaxies using both optical and near infrared surface brightness have not found any excess of bars relative to quiescent galaxies, the searches have not been able to rule out small-scale nuclear bars. To look for these nuclear bars we use HST WFPC2-NICMOS color maps to search for the straight dust lane signature of strong bars. Of the twelve Seyfert galaxies in our sample, only three have dust lanes consistent with a strong nuclear bar. Therefore, strong arXiv:astro-ph/9903053v1 3 Mar 1999 nuclear bars cannot be the primary fueling mechanism for Seyfert nuclei. We do find that a majority of the galaxies show an spiral morphology in their dust lanes. These spiral arms may be a possible fueling mechanism. Subject headings: galaxies: Seyfert — galaxies: ISM — galaxies: nuclei 1Based on observations with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc.