June 2018 Volume 25, Number 6
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Kinematics of Planetary Nebulae in M51's Tidal Debris
Draft version December 17, 2018 A Preprint typeset using L TEX style emulateapj v. 14/09/00 KINEMATICS OF PLANETARY NEBULAE IN M51’S TIDAL DEBRIS Patrick R. Durrell [email protected] Department of Astronomy and Astrophysics, Penn State University, 525 Davey Lab, University Park, PA 16802 J. Christopher Mihos1, John J. Feldmeier [email protected], [email protected] Department of Astronomy, Case Western Reserve University, 10900 Euclid Ave, Cleveland, OH 44106 George H. Jacoby [email protected] WIYN Observatory2, P.O. Box 26732, Tucson AZ 85726 and Robin Ciardullo [email protected] Department of Astronomy and Astrophysics, Penn State University, 525 Davey Lab, University Park, PA 16802 accepted for publication in the Astrophysical Journal ABSTRACT We report the results of a radial velocity survey of planetary nebulae (PNe) located in the tidal features of the well-known interacting system NGC 5194/95 (M51). We find clear kinematic evidence that M51’s northwestern tidal debris consists of two discrete structures which overlap in projection – NGC 5195’s own tidal tail, and diffuse material stripped from NGC 5194. We compare these kinematic data to a new numerical simulation of the M51 system, and show that the data are consistent with the classic “single passage” model for the encounter, with a parabolic satellite trajectory and a 2:1 mass ratio. We also comment on the spectra of two unusual objects: a high-velocity PN which may be associated with NGC 5194’s halo, and a possible interloping high-redshift galaxy. Subject headings: galaxies: individual (M51) — galaxies: interactions — galaxies: kinematics and dynamics — planetary nebulae: general 1. -
Messier Objects
Messier Objects From the Stocker Astroscience Center at Florida International University Miami Florida The Messier Project Main contributors: • Daniel Puentes • Steven Revesz • Bobby Martinez Charles Messier • Gabriel Salazar • Riya Gandhi • Dr. James Webb – Director, Stocker Astroscience center • All images reduced and combined using MIRA image processing software. (Mirametrics) What are Messier Objects? • Messier objects are a list of astronomical sources compiled by Charles Messier, an 18th and early 19th century astronomer. He created a list of distracting objects to avoid while comet hunting. This list now contains over 110 objects, many of which are the most famous astronomical bodies known. The list contains planetary nebula, star clusters, and other galaxies. - Bobby Martinez The Telescope The telescope used to take these images is an Astronomical Consultants and Equipment (ACE) 24- inch (0.61-meter) Ritchey-Chretien reflecting telescope. It has a focal ratio of F6.2 and is supported on a structure independent of the building that houses it. It is equipped with a Finger Lakes 1kx1k CCD camera cooled to -30o C at the Cassegrain focus. It is equipped with dual filter wheels, the first containing UBVRI scientific filters and the second RGBL color filters. Messier 1 Found 6,500 light years away in the constellation of Taurus, the Crab Nebula (known as M1) is a supernova remnant. The original supernova that formed the crab nebula was observed by Chinese, Japanese and Arab astronomers in 1054 AD as an incredibly bright “Guest star” which was visible for over twenty-two months. The supernova that produced the Crab Nebula is thought to have been an evolved star roughly ten times more massive than the Sun. -
Do Normal Galaxies Host a Black Hole? the High Energy Perspective
DO NORMAL GALAXIES HOST A BLACK HOLE? THE HIGH ENERGY PERSPECTIVE 1 Y. Terashima2 Nagoya University ABSTRACT We review ASCA results on a search for low luminosity active nuclei at the center of nearby normal galaxies. More than a dozen low-luminosity AGN have been discovered with 2–10 keV − − luminosity in the range 1040 41 ergs s 1. Their X-ray properties are in some respects similar to those of luminous Seyfert galaxies, but differ in other respects. We also present estimated black hole masses in low luminosity AGNs and a drastic activity decline in the nucleus of the radio galaxy Fornax A. These results altogether suggest that relics of the past luminous AGNs lurk in nearby normal galaxies. KEYWORDS: Galaxies; Low luminosity AGNs; LINERs; Black holes 1. Introduction The number density of quasars is peaked at a redshift of z ∼ 2 and rapidly de- creases toward smaller redshifts. In the local universe, there is no AGN emitting at huge luminosity like quasars. These facts infer that quasars evolve to supermassive black holes in nearby apparently normal galaxies (e.g. Rees 1990). The growing evidence for supermassive black holes in nearby galaxies are ob- tained from recent optical and radio observations of gas/stellar kinematics around the center of galaxies (e.g. Ho 1998a; Magorrian et al. 1998; Kormendy & Rich- stone 1995). If fueling to the supermassive black hole takes place with a small arXiv:astro-ph/9905218v1 17 May 1999 mass accretion rate, they are expected to be observed as very low luminosity AGNs compared to quasars. Recent optical spectroscopic surveys have shown that low level activity is fairly common in nearby galaxies. -
What's in This Issue?
A JPL Image of surface of Mars, and JPL Ingenuity Helicioptor illustration. July 11th at 4:00 PM, a family barbeque at HRPO!!! This is in lieu of our regular monthly meeting.) (Monthly meetings are on 2nd Mondays at Highland Road Park Observatory) This is a pot-luck. Club will provide briskett and beverages, others will contribute as the spirit moves. What's In This Issue? President’s Message Member Meeting Minutes Business Meeting Minutes Outreach Report Asteroid and Comet News Light Pollution Committee Report Globe at Night SubReddit and Discord BRAS Member Astrophotos ARTICLE: Astrophotography with your Smart Phone Observing Notes: Canes Venatici – The Hunting Dogs Like this newsletter? See PAST ISSUES online back to 2009 Visit us on Facebook – Baton Rouge Astronomical Society BRAS YouTube Channel Baton Rouge Astronomical Society Newsletter, Night Visions Page 2 of 23 July 2021 President’s Message Hey everybody, happy fourth of July. I hope ya’ll’ve remembered your favorite coping mechanism for dealing with the long hot summers we have down here in the bayou state, or, at the very least, are making peace with the short nights that keep us from enjoying both a good night’s sleep and a productive observing/imaging session (as if we ever could get a long enough break from the rain for that to happen anyway). At any rate, we figured now would be as good a time as any to get the gang back together for a good old fashioned potluck style barbecue: to that end, we’ve moved the July meeting to the Sunday, 11 July at 4PM at HRPO. -
WALLABY – an SKA Pathfinder H I Survey
University of Louisville ThinkIR: The University of Louisville's Institutional Repository Faculty Scholarship 7-1-2020 WALLABY – an SKA Pathfinder H i survey Bärbel S. Koribalski Australia Telescope National Facility L. Staveley-Smith ARC Centre of Excellence for All-sky Astrophysics T. Westmeier ARC Centre of Excellence for All-sky Astrophysics P. Serra Osservatorio Astronomico di Cagliari K. Spekkens Royal Military College of Canada See next page for additional authors Follow this and additional works at: https://ir.library.louisville.edu/faculty Part of the Astrophysics and Astronomy Commons ThinkIR Citation Koribalski, Bärbel S.; Staveley-Smith, L.; Westmeier, T.; Serra, P.; Spekkens, K.; Wong, O. I.; Lee-Waddell, K.; Lagos, C. D.P.; Obreschkow, D.; Ryan-Weber, E. V.; Zwaan, M.; Kilborn, V.; Bekiaris, G.; Bekki, K.; Bigiel, F.; Boselli, A.; Bosma, A.; Catinella, B.; Chauhan, G.; Cluver, M. E.; Colless, M.; Courtois, H. M.; Crain, R. A.; de Blok, W. J.G.; Dénes, H.; Duffy, A. R.; Elagali, A.; Fluke, C. J.; For, B. Q.; Heald, G.; Henning, P. A.; Hess, K. M.; and Holwerda, Benne W., "WALLABY – an SKA Pathfinder H i survey" (2020). Faculty Scholarship. 476. https://ir.library.louisville.edu/faculty/476 This Article is brought to you for free and open access by ThinkIR: The University of Louisville's Institutional Repository. It has been accepted for inclusion in Faculty Scholarship by an authorized administrator of ThinkIR: The University of Louisville's Institutional Repository. For more information, please contact [email protected]. Authors Bärbel S. Koribalski, L. Staveley-Smith, T. Westmeier, P. Serra, K. Spekkens, O. -
Lord Rosse, Robinson, South and the Discovery of Spiral Structure in 1845
Journal of Astronomical History and Heritage, 15(1), 19-29 (2012). THE M51 MYSTERY: LORD ROSSE, ROBINSON, SOUTH AND THE DISCOVERY OF SPIRAL STRUCTURE IN 1845 Wolfgang Steinicke Gottenheimerstr. 18, D-79224, Umkirch, Germany. E-mail: [email protected] Abstract: In April 1845 Lord Rosse discovered the spiral structure of M51 with his 72-inch reflector at Birr Castle. Already in March the new telescope had been pointed at the object in Canes Venatici, later nicknamed the ‘Whirlpool Nebula’. Two experienced astronomers were present: Sir James South and the Reverend Thomas Romney Robin- son. The problem is that there is no record that they noticed the spiral structure, even though it was immediately seen by Lord Rosse the next month. The solution presented here is based on evidentiary facts, highlighting the nine- teenth century astronomical praxis. Focal points are bias, fantasy and a sometimes fatal conspiracy of eye and brain. Keywords: Spiral structure, nebulae, star clusters, Lord Rosse, Birr Castle, Leviathan of Parsonstown, Whirlpool Nebula, nebular hypothesis, visual observation, drawings. 1 DISCOVERY OF M51 AND JOHN the core, surrounded by a divided ring (Figure 2); it HERSCHEL’S ‘RING NEBULA’ appears as Figure 25 in the Slough catalogue. Herschel M51 (NGC 5194) is a nearby Sbc-galaxy with a visual magnitude 8.4 and a size of 11.2 × 6.9. It was dis- covered on 13 October 1773 by Charles Messier (1730–1817) with a 3.5-inch refractor at Paris. The description, published in his famous catalogue of 1781, reads: “… very faint nebula without stars …” 1 (Messier, 1781: 247). -
The Unveiling of the Newly Discovered Vela Supercluster 1
The Unveiling of the newly discovered Vela Supercluster ∗ PoS(SSC2015)040 Renée C. Kraan-Korteweg†, Thomas H. Jarrett and Ahmed Elagali Astrophysics, Cosmology and Gravity Centre, University of Cape Town, 7701 Rondebosch, South Africa E-mail: [email protected] Michelle E. Cluver Department of Physics, University of the Western Cape, Bellville, South Africa Maciej Bilicki Astrophysics, Cosmology and Gravity Centre, University of Cape Town, 7701 Rondebosch, South Africa & Leiden Observatory, Leiden University, The Netherlands Matthew M. Colless Research School of Astronomy and Astrophysics, Australian National University, Canberra, Australia Multi-object spectroscopic observations of high density galaxy concentrations were obtained be- tween 2012 and 2014 with SALT, using the multi-object spectrometer (MOS) of the Robert Stobie Spectograph (RSS) on SALT. The goal was to find the missing clusters in an earlier identified ex- tended galaxy overdensity centered at ∼ 18000 km s−1 located at low Galactic latitudes in Vela. Reliable redshifts could be extracted for ∼ 80% of the targeted, highly-obscured galaxies. They were found to have an accuracy of the order of s ∼ 150 km s−1. Of the 13 observed fields, ten revealed clear signatures of galaxy clusters. The majority of the clusters form part of the Vela overdensity. Their distribution also confirmed our suspicion that the Vela overdensity is even more extended and seems to straddle the Galactic Plane. Subsequent multi-fibre spectroscopy with AAOmega+2dF on the Australian Telescope confirmed that these clusters are embedded in a gigantic overdensity of about 20◦ ×20◦ on the sky. The overdensity and its clusters show strong similarities to massive superclusters such as the Shapley Supercluster. -
Annual Report / Rapport Annuel / Jahresbericht 1996
Annual Report / Rapport annuel / Jahresbericht 1996 ✦ ✦ ✦ E U R O P E A N S O U T H E R N O B S E R V A T O R Y ES O✦ 99 COVER COUVERTURE UMSCHLAG Beta Pictoris, as observed in scattered light Beta Pictoris, observée en lumière diffusée Beta Pictoris, im Streulicht bei 1,25 µm (J- at 1.25 microns (J band) with the ESO à 1,25 microns (bande J) avec le système Band) beobachtet mit dem adaptiven opti- ADONIS adaptive optics system at the 3.6-m d’optique adaptative de l’ESO, ADONIS, au schen System ADONIS am ESO-3,6-m-Tele- telescope and the Observatoire de Grenoble télescope de 3,60 m et le coronographe de skop und dem Koronographen des Obser- coronograph. l’observatoire de Grenoble. vatoriums von Grenoble. The combination of high angular resolution La combinaison de haute résolution angu- Die Kombination von hoher Winkelauflö- (0.12 arcsec) and high dynamical range laire (0,12 arcsec) et de gamme dynamique sung (0,12 Bogensekunden) und hohem dy- (105) allows to image the disk to only 24 AU élevée (105) permet de reproduire le disque namischen Bereich (105) erlaubt es, die from the star. Inside 50 AU, the main plane jusqu’à seulement 24 UA de l’étoile. A Scheibe bis zu einem Abstand von nur 24 AE of the disk is inclined with respect to the l’intérieur de 50 UA, le plan principal du vom Stern abzubilden. Innerhalb von 50 AE outer part. Observers: J.-L. Beuzit, A.-M. -
A Kinematic Confirmation of the Hidden Vela Supercluster
MNRAS 000,1{6 (2019) Preprint 20 September 2019 Compiled using MNRAS LATEX style file v3.0 A kinematic confirmation of the hidden Vela supercluster H´el`ene M. Courtois1?, Ren´ee C. Kraan-Korteweg2, Alexandra Dupuy1, Romain Graziani1 and Noam I. Libeskind,1;3 1University of Lyon, UCB Lyon 1, CNRS/IN2P3, IP2I Lyon, France 2Department of Astronomy, University of Cape Town, Private Bag X3, 7701 Rondebosch, South Africa 3Leibniz-Institut fur¨ Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany Accepted....... ; ABSTRACT The universe region obscured by the Milky Way is very large and only future blind large HI redshift, and targeted peculiar surveys on the outer borders will determine how much mass is hidden there. Meanwhile, we apply for the first time two independent techniques to the galaxy peculiar velocity catalog CosmicF lows−3 in order to explore for the kinematic signature of a specific large-scale structure hidden behind this zone : the Vela supercluster at cz ∼ 18; 000,km s−1 . Using the gravitational velocity and density contrast fields, we find excellent agreement when comparing our results to the Vela object as traced in redshift space. The article provides the first kinematic evidence of a major mass concentration (knot of the Cosmic Web) located in the direction behind Vela constellation, pin-pointing that the Zone of Avoidance should be surveyed in detail in the future . Key words: large-scale structure of Universe 1 INTRODUCTION (sgl; sgb ∼ 173◦; −47◦)(Kraan-Korteweg et al.(2017, 2015), henceforth KK17a,b). A significant bulk flow residual was revealed in 2014 in the Radial peculiar velocities can be modeled using the analysis of the 6dF peculiar velocity survey based on 8,885 Wiener filter methodology Zaroubi et al.(1999); Hoffman galaxies in the southern hemisphere within a volume cz (2009); Courtois et al.(2012), recently re-vamped by data ≤ 16; 000 km s−1 Springob et al.(2014). -
Large-Scale Structures Behind the Southern Milky Way From
Large-Scale Structures Behind the Southern Milky Way from Observations of Partially Obscured Galaxies R.C. Kraan-Korteweg Observatoire de Paris-Meudon, D.A.E.C., 92195 Meudon Cedex, France [email protected] P.A. Woudt Dept. of Astronomy, University of Cape Town, Rondebosch 7700, South Africa P.A. Henning Dept. of Physics and Astronomy, University of New Mexico, Albuquerque, USA Abstract We report here on extragalactic large-scale structures uncovered by a deep optical survey for galaxies behind the southern Milky Way. Systematic visual inspection of the ESO/SRC- ◦ ◦ survey revealed over 10000 previously unknown galaxies in the region 265 ∼<ℓ ∼< 340 , |b| ∼< 10◦. With subsequently obtained redshifts of more than 10% of these galaxies, new structures across the Milky Way are unveiled, such as a filament at v ∼ 2500 km s−1 connecting to the Hydra and Antlia clusters, a shallow extended supercluster in Vela (∼ 6000 km s−1), and a −1 15 nearby (4882 km s ), very massive (M ∼ 2 − 5 · 10 M⊙), rich Coma-like cluster which seems to constitute the previously unidentified center of the Great Attractor. The innermost part of the Milky Way where the foreground obscuration in the blue is m 21 −2 AB ∼> 5 , respectively H I-column densities NH I ∼> 6·10 cm remains fully opaque. In this approximately 8◦ wide strip, the forthcoming blind H I-survey with the multi-beam system at Parkes will provide the only tool to unveil this part of the extragalactic sky. Keywords: galaxies: distances and redshifts - large-scale structure of Universe - surveys arXiv:astro-ph/9611099v1 13 Nov 1996 1 Introduction The Milky Way obscures about 25% of the extragalactic sky. -
00E the Construction of the Universe Symphony
The basic construction of the Universe Symphony. There are 30 asterisms (Suites) in the Universe Symphony. I divided the asterisms into 15 groups. The asterisms in the same group, lay close to each other. Asterisms!! in Constellation!Stars!Objects nearby 01 The W!!!Cassiopeia!!Segin !!!!!!!Ruchbah !!!!!!!Marj !!!!!!!Schedar !!!!!!!Caph !!!!!!!!!Sailboat Cluster !!!!!!!!!Gamma Cassiopeia Nebula !!!!!!!!!NGC 129 !!!!!!!!!M 103 !!!!!!!!!NGC 637 !!!!!!!!!NGC 654 !!!!!!!!!NGC 659 !!!!!!!!!PacMan Nebula !!!!!!!!!Owl Cluster !!!!!!!!!NGC 663 Asterisms!! in Constellation!Stars!!Objects nearby 02 Northern Fly!!Aries!!!41 Arietis !!!!!!!39 Arietis!!! !!!!!!!35 Arietis !!!!!!!!!!NGC 1056 02 Whale’s Head!!Cetus!! ! Menkar !!!!!!!Lambda Ceti! !!!!!!!Mu Ceti !!!!!!!Xi2 Ceti !!!!!!!Kaffalijidhma !!!!!!!!!!IC 302 !!!!!!!!!!NGC 990 !!!!!!!!!!NGC 1024 !!!!!!!!!!NGC 1026 !!!!!!!!!!NGC 1070 !!!!!!!!!!NGC 1085 !!!!!!!!!!NGC 1107 !!!!!!!!!!NGC 1137 !!!!!!!!!!NGC 1143 !!!!!!!!!!NGC 1144 !!!!!!!!!!NGC 1153 Asterisms!! in Constellation Stars!!Objects nearby 03 Hyades!!!Taurus! Aldebaran !!!!!! Theta 2 Tauri !!!!!! Gamma Tauri !!!!!! Delta 1 Tauri !!!!!! Epsilon Tauri !!!!!!!!!Struve’s Lost Nebula !!!!!!!!!Hind’s Variable Nebula !!!!!!!!!IC 374 03 Kids!!!Auriga! Almaaz !!!!!! Hoedus II !!!!!! Hoedus I !!!!!!!!!The Kite Cluster !!!!!!!!!IC 397 03 Pleiades!! ! Taurus! Pleione (Seven Sisters)!! ! ! Atlas !!!!!! Alcyone !!!!!! Merope !!!!!! Electra !!!!!! Celaeno !!!!!! Taygeta !!!!!! Asterope !!!!!! Maia !!!!!!!!!Maia Nebula !!!!!!!!!Merope Nebula !!!!!!!!!Merope -
Canes Venatici I Cloud of Galaxies Seen in the Hα Line
A&A 479, 603–624 (2008) Astronomy DOI: 10.1051/0004-6361:20078652 & c ESO 2008 Astrophysics Canes Venatici I cloud of galaxies seen in the Hα line S. S. Kaisin and I. D. Karachentsev Special Astrophysical Observatory, Russian Academy of Sciences, N. Arkhyz, KChR, 369167, Russia e-mail: [email protected] Received 11 September 2007 / Accepted 25 September 2007 ABSTRACT We present results of Hα imaging for 42 galaxies in the nearby low-density cloud Canes Venatici I, populated mainly by late-type objects. Estimates of the Hα flux and integrated star formation rate (SFR) are now available for all 78 known members of this scattered system, spanning a large range in luminosity, surface brightness, HI content and SFR. Distributions of the CVnI galaxies versus their SFR, blue absolute magnitude and total hydrogen mass, are given in comparison with those for a population of the nearby virialized group around M 81. We found no essential correlation between star formation activity in a galaxy and its density environment. The bulk of CVnI galaxies had enough time to generate their baryon mass with the observed SFR. Most of them also possess a supply of gas that is sufficient to maintain their observed SFRs during the next Hubble time. Key words. galaxies: evolution – galaxies: ISM – galaxies: dwarf 1. Introduction 2. Observations and data reduction The distribution over the sky of 500 galaxies of the Local CCD images in the Hα-line and continuum were obtained for Volume, with distances within 10 Mpc, shows considerable in- 42 galaxies of the CVnI cloud during observing runs from March homogeneities due to the presence of groups and voids.