Norfolk Astronomical Society May 2013 Monthly Sky Calendar
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BRAS Newsletter August 2013
www.brastro.org August 2013 Next meeting Aug 12th 7:00PM at the HRPO Dark Site Observing Dates: Primary on Aug. 3rd, Secondary on Aug. 10th Photo credit: Saturn taken on 20” OGS + Orion Starshoot - Ben Toman 1 What's in this issue: PRESIDENT'S MESSAGE....................................................................................................................3 NOTES FROM THE VICE PRESIDENT ............................................................................................4 MESSAGE FROM THE HRPO …....................................................................................................5 MONTHLY OBSERVING NOTES ....................................................................................................6 OUTREACH CHAIRPERSON’S NOTES .........................................................................................13 MEMBERSHIP APPLICATION .......................................................................................................14 2 PRESIDENT'S MESSAGE Hi Everyone, I hope you’ve been having a great Summer so far and had luck beating the heat as much as possible. The weather sure hasn’t been cooperative for observing, though! First I have a pretty cool announcement. Thanks to the efforts of club member Walt Cooney, there are 5 newly named asteroids in the sky. (53256) Sinitiere - Named for former BRAS Treasurer Bob Sinitiere (74439) Brenden - Named for founding member Craig Brenden (85878) Guzik - Named for LSU professor T. Greg Guzik (101722) Pursell - Named for founding member Wally Pursell -
Infrared Spectroscopy of Nearby Radio Active Elliptical Galaxies
The Astrophysical Journal Supplement Series, 203:14 (11pp), 2012 November doi:10.1088/0067-0049/203/1/14 C 2012. The American Astronomical Society. All rights reserved. Printed in the U.S.A. INFRARED SPECTROSCOPY OF NEARBY RADIO ACTIVE ELLIPTICAL GALAXIES Jeremy Mould1,2,9, Tristan Reynolds3, Tony Readhead4, David Floyd5, Buell Jannuzi6, Garret Cotter7, Laura Ferrarese8, Keith Matthews4, David Atlee6, and Michael Brown5 1 Centre for Astrophysics and Supercomputing Swinburne University, Hawthorn, Vic 3122, Australia; [email protected] 2 ARC Centre of Excellence for All-sky Astrophysics (CAASTRO) 3 School of Physics, University of Melbourne, Melbourne, Vic 3100, Australia 4 Palomar Observatory, California Institute of Technology 249-17, Pasadena, CA 91125 5 School of Physics, Monash University, Clayton, Vic 3800, Australia 6 Steward Observatory, University of Arizona (formerly at NOAO), Tucson, AZ 85719 7 Department of Physics, University of Oxford, Denys, Oxford, Keble Road, OX13RH, UK 8 Herzberg Institute of Astrophysics Herzberg, Saanich Road, Victoria V8X4M6, Canada Received 2012 June 6; accepted 2012 September 26; published 2012 November 1 ABSTRACT In preparation for a study of their circumnuclear gas we have surveyed 60% of a complete sample of elliptical galaxies within 75 Mpc that are radio sources. Some 20% of our nuclear spectra have infrared emission lines, mostly Paschen lines, Brackett γ , and [Fe ii]. We consider the influence of radio power and black hole mass in relation to the spectra. Access to the spectra is provided here as a community resource. Key words: galaxies: elliptical and lenticular, cD – galaxies: nuclei – infrared: general – radio continuum: galaxies ∼ 1. INTRODUCTION 30% of the most massive galaxies are radio continuum sources (e.g., Fabbiano et al. -
Messier Plus Marathon Text
Messier Plus Marathon Object List by Wally Brown & Bob Buckner with additional objects by Mike Roos Object Data - Saguaro Astronomy Club Score is most numbered objects in a single night. Tiebreaker is count of un-numbered objects Observer Name Date Address Marathon Obects __________ Tiebreaker Objects ________ SEQ OBJECT TYPE CON R.A. DEC. RISE TRANSIT SET MAG SIZE NOTES TIME M 53 GLOCL COM 1312.9 +1810 7:21 14:17 21:12 7.7 13.0' NGC 5024, !B,vC,iR,vvmbM,st 12.. NGC 5272, !!,eB,vL,vsmbM,st 11.., Lord Rosse-sev dark 1 M 3 GLOCL CVN 1342.2 +2822 7:11 14:46 22:20 6.3 18.0' marks within 5' of center 2 M 5 GLOCL SER 1518.5 +0205 10:17 16:22 22:27 5.7 23.0' NGC 5904, !!,vB,L,eCM,eRi, st mags 11...;superb cluster M 94 GALXY CVN 1250.9 +4107 5:12 13:55 22:37 8.1 14.4'x12.1' NGC 4736, vB,L,iR,vsvmbM,BN,r NGC 6121, Cl,8 or 10 B* in line,rrr, Look for central bar M 4 GLOCL SCO 1623.6 -2631 12:56 17:27 21:58 5.4 36.0' structure M 80 GLOCL SCO 1617.0 -2258 12:36 17:21 22:06 7.3 10.0' NGC 6093, st 14..., Extremely rich and compressed M 62 GLOCL OPH 1701.2 -3006 13:49 18:05 22:21 6.4 15.0' NGC 6266, vB,L,gmbM,rrr, Asymmetrical M 19 GLOCL OPH 1702.6 -2615 13:34 18:06 22:38 6.8 17.0' NGC 6273, vB,L,R,vCM,rrr, One of the most oblate GC 3 M 107 GLOCL OPH 1632.5 -1303 12:17 17:36 22:55 7.8 13.0' NGC 6171, L,vRi,vmC,R,rrr, H VI 40 M 106 GALXY CVN 1218.9 +4718 3:46 13:23 22:59 8.3 18.6'x7.2' NGC 4258, !,vB,vL,vmE0,sbMBN, H V 43 M 63 GALXY CVN 1315.8 +4201 5:31 14:19 23:08 8.5 12.6'x7.2' NGC 5055, BN, vsvB stell. -
Winter Constellations
Winter Constellations *Orion *Canis Major *Monoceros *Canis Minor *Gemini *Auriga *Taurus *Eradinus *Lepus *Monoceros *Cancer *Lynx *Ursa Major *Ursa Minor *Draco *Camelopardalis *Cassiopeia *Cepheus *Andromeda *Perseus *Lacerta *Pegasus *Triangulum *Aries *Pisces *Cetus *Leo (rising) *Hydra (rising) *Canes Venatici (rising) Orion--Myth: Orion, the great hunter. In one myth, Orion boasted he would kill all the wild animals on the earth. But, the earth goddess Gaia, who was the protector of all animals, produced a gigantic scorpion, whose body was so heavily encased that Orion was unable to pierce through the armour, and was himself stung to death. His companion Artemis was greatly saddened and arranged for Orion to be immortalised among the stars. Scorpius, the scorpion, was placed on the opposite side of the sky so that Orion would never be hurt by it again. To this day, Orion is never seen in the sky at the same time as Scorpius. DSO’s ● ***M42 “Orion Nebula” (Neb) with Trapezium A stellar nursery where new stars are being born, perhaps a thousand stars. These are immense clouds of interstellar gas and dust collapse inward to form stars, mainly of ionized hydrogen which gives off the red glow so dominant, and also ionized greenish oxygen gas. The youngest stars may be less than 300,000 years old, even as young as 10,000 years old (compared to the Sun, 4.6 billion years old). 1300 ly. 1 ● *M43--(Neb) “De Marin’s Nebula” The star-forming “comma-shaped” region connected to the Orion Nebula. ● *M78--(Neb) Hard to see. A star-forming region connected to the Orion Nebula. -
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. -
A Gaia DR2 View of the Open Cluster Population in the Milky Way T
Astronomy & Astrophysics manuscript no. manuscript˙arXiv2 © ESO 2018 July 13, 2018 A Gaia DR2 view of the Open Cluster population in the Milky Way T. Cantat-Gaudin1, C. Jordi1, A. Vallenari2, A. Bragaglia3, L. Balaguer-Nu´nez˜ 1, C. Soubiran4, D. Bossini2, A. Moitinho5, A. Castro-Ginard1, A. Krone-Martins5, L. Casamiquela4, R. Sordo2, and R. Carrera2 1 Institut de Ciencies` del Cosmos, Universitat de Barcelona (IEEC-UB), Mart´ı i Franques` 1, E-08028 Barcelona, Spain 2 INAF-Osservatorio Astronomico di Padova, vicolo Osservatorio 5, 35122 Padova, Italy 3 INAF-Osservatorio di Astrofisica e Scienza dello Spazio, via Gobetti 93/3, 40129 Bologna, Italy 4 Laboratoire dAstrophysique de Bordeaux, Univ. Bordeaux, CNRS, UMR 5804, 33615 Pessac, France 5 CENTRA, Faculdade de Ciencias,ˆ Universidade de Lisboa, Ed. C8, Campo Grande, P-1749-016 Lisboa, Portugal Received date / Accepted date ABSTRACT Context. Open clusters are convenient probes of the structure and history of the Galactic disk. They are also fundamental to stellar evolution studies. The second Gaia data release contains precise astrometry at the sub-milliarcsecond level and homogeneous pho- tometry at the mmag level, that can be used to characterise a large number of clusters over the entire sky. Aims. In this study we aim to establish a list of members and derive mean parameters, in particular distances, for as many clusters as possible, making use of Gaia data alone. Methods. We compile a list of thousands of known or putative clusters from the literature. We then apply an unsupervised membership assignment code, UPMASK, to the Gaia DR2 data contained within the fields of those clusters. -
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). -
Disney Pixar CARS Finders Guide
Open Star Clusters A Guide for the Open Star Cluster Observing Club Astronomical League Open Star Clusters NGC 6520 (left) and B 86 (right) Cover: M45 Courtesy of Russell Croman A Selection of 125 Open Star Clusters By Benjamin Jones Astronomical League Copyright 2005 by the Astronomical League First Printing 2007 No part of this publication may be reproduced or utilized in any form or by any means, electronic or mechanical, including photocopying, recording, or by an information storage and retrieval system without permission in writing from the Astronomical League. Limited permission is granted for the downloading, reproducing, and/or printing of the material for personal use. Astronomical League 9201 Ward Parkway, Suite 100 Kansas City, MO 64114 816-DEEP SKY www.astroleague.org References: http://www.geocities.com/ariane1au/Page030.htm Star Clusters by Brent A. Archinal and Steven J. Hynes, published by Willmann-Bell Publishing, 2003. Pictures under the Trumpler Classification examples referenced to the Digital Sky Survey. The Digitized Sky Surveys were produced at the Space Telescope Science Institute under U.S. Government grant NAG W-2166. The images of these surveys are based on photographic data obtained using the Oschin Schmidt Telescope on Palomar Mountain and the UK Schmidt Telescope. The plates were processed into the present compressed digital form with the permission of these institutions. i Acknowledgements The author would like to thank the following people for their help with this program. Without their assistance, this program would have never been created. Sue French, Dr. Brent Archinal, John Wagoner, Mikkel Stein, Becky Ramotowski, and Michael Hotka. -
Übersicht NGC-Objektauswahl Cepheus Zur Übersichtskarte
NGC-Objektauswahl Cepheus NGC 40 NGC 7055 NGC 7354 NGC 188 NGC 7076 NGC 7380 NGC 1184 NGC 7129 NGC 7419 NGC 1544 NGC 7139 NGC 7423 NGC 2276 NGC 7142 NGC 7429 NGC 2300 NGC 7160 NGC 7510 NGC 6939 NGC 7226 NGC 7538 NGC 6949 NGC 7235 NGC 7708 NGC 6951 NGC 7261 NGC 7762 NGC 7023 NGC 7281 NGC 7822 Sternbild- Übersicht Zur Objektauswahl: Nummer anklicken Zur Übersichtskarte: Objekt anklicken Sternbildübersicht Auswahl NGC 40_7708 Aufsuchkarte Auswahl NGC 188_Aufsuchkarte 2 UMi 2 Auswahl NGC 1184 Aufsuchkarte Auswahl NGC 1544_2276_2300 Aufsuchkarte Auswahl NGC 6939 Aufsuchkarte Auswahl NGC 6949_6951 Aufsuchkarte Auswahl NGC 7023 Aufsuchkarte Auswahl NGC 7055 Aufsuchkarte Auswahl NGC 7076 Aufsuchkarte Auswahl NGC 7129_7142 Aufsuchkarte Auswahl NGC 7139_7160 Aufsuchkarte Auswahl NGC 7226_7235 Aufsuchkarte Auswahl N 7261_7281 Aufsuchkarte Auswahl NGC 7354_7419_7429_7510_7538 Aufsuchkarte Auswahl NGC 7380_7423 Aufsuchkarte Auswahl NGC 7762_7822 Aufsuchkarte Auswahl NGC 40 Übersichtskarte Aufsuch- Auswahl karte NGC 188 Übersichtskarte Aufsuch- Auswahl karte NGC 1184 Übersichtskarte Aufsuch- Auswahl karte NGC 1544 Übersichtskarte Aufsuch- Auswahl karte N 2276_N 2300 Übersichtskarte Aufsuch- Auswahl karte NGC 6939 Übersichtskarte Aufsuch- Auswahl karte NGC 6949 Übersichtskarte Aufsuch- Auswahl karte NGC 6951 Übersichtskarte Aufsuch- Auswahl karte NGC 7023 Übersichtskarte Aufsuch- Auswahl karte NGC 7055 Übersichtskarte Aufsuch- Auswahl karte NGC 7076 Übersichtskarte Aufsuch- Auswahl karte NGC 7129_7142 Übersichtskarte Aufsuch- Auswahl karte NGC 7139 -
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. -
A Search For" Dwarf" Seyfert Nuclei. VII. a Catalog of Central Stellar
TO APPEAR IN The Astrophysical Journal Supplement Series. Preprint typeset using LATEX style emulateapj v. 26/01/00 A SEARCH FOR “DWARF” SEYFERT NUCLEI. VII. A CATALOG OF CENTRAL STELLAR VELOCITY DISPERSIONS OF NEARBY GALAXIES LUIS C. HO The Observatories of the Carnegie Institution of Washington, 813 Santa Barbara St., Pasadena, CA 91101 JENNY E. GREENE1 Department of Astrophysical Sciences, Princeton University, Princeton, NJ ALEXEI V. FILIPPENKO Department of Astronomy, University of California, Berkeley, CA 94720-3411 AND WALLACE L. W. SARGENT Palomar Observatory, California Institute of Technology, MS 105-24, Pasadena, CA 91125 To appear in The Astrophysical Journal Supplement Series. ABSTRACT We present new central stellar velocity dispersion measurements for 428 galaxies in the Palomar spectroscopic survey of bright, northern galaxies. Of these, 142 have no previously published measurements, most being rela- −1 tively late-type systems with low velocity dispersions (∼<100kms ). We provide updates to a number of literature dispersions with large uncertainties. Our measurements are based on a direct pixel-fitting technique that can ac- commodate composite stellar populations by calculating an optimal linear combination of input stellar templates. The original Palomar survey data were taken under conditions that are not ideally suited for deriving stellar veloc- ity dispersions for galaxies with a wide range of Hubble types. We describe an effective strategy to circumvent this complication and demonstrate that we can still obtain reliable velocity dispersions for this sample of well-studied nearby galaxies. Subject headings: galaxies: active — galaxies: kinematics and dynamics — galaxies: nuclei — galaxies: Seyfert — galaxies: starburst — surveys 1. INTRODUCTION tors, apertures, observing strategies, and analysis techniques. -
MASSIVE Galaxies with Supermassive Black Holes
Hubble Space Telescope Cycle 23 GO Proposal 750 Homogeneous Distances and Central Profiles for MASSIVE Survey Galaxies with Supermassive Black Holes Scientific Category: UNRESOLVED STELLAR POPULATIONS AND GALAXY STRUCTURE Scientific Keywords: Black Holes, Cosmological Parameters And Distance Scale, Galaxy Centers, Galaxy Morphology And Structure Instruments: WFC3 Proprietary Period: 12 Proposal Size: Small Orbit Request Prime Parallel Cycle 23 34 0 Abstract Massive early-type galaxies are the subject of intense interest: they exhibit the most massive black holes (BHs), most extreme stellar IMFs, and most dramatic size evolution over cosmic time. Yet, their complex formation histories remain obscure. Enter MASSIVE: a volume-limited survey of the structure and dynamics of the 100 most massive early-type galaxies within ~100 Mpc. We use integral-field spectroscopy (IFS) on sub-arcsecond (with AO) and large scales for simultaneous dynamical modeling of the supermassive BH, stars, and dark matter. The goals of MASSIVE include precise constraints on BH-galaxy scaling relations, the stellar IMF, and late-time assembly of ellipticals. We have already obtained much of the needed IFS and wide-field imaging for this project; here, we propose to add the one missing ingredient: high-resolution imaging with HST. This will nail down the central profiles, greatly reducing the degeneracy between M/L and BH masses in our dynamical orbit modeling. Further, we will measure efficient, high-quality WFC3/IR SBF distances for all targets, thereby removing potentially large errors from peculiar velocities (especially in the high-density regions occupied by massive early-types) or heterogeneous distance methods. Distance errors are insidious: they affect BH masses and galaxy properties in dissimilar ways, and thus can bias both the scatter and slopes of the scaling relations.