December 2017 BRAS Newsletter
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Black Holes in 4 Nearby Radio Galaxies
Astrophys Space Sci (2015) 356:347–351 DOI 10.1007/s10509-014-2166-6 ORIGINAL ARTICLE Black holes in 4 nearby radio galaxies Jeremy Mould · Tony Readhead · Garret Cotter · David Batt · Mark Durré Received: 26 June 2014 / Accepted: 18 October 2014 / Published online: 4 March 2015 © Springer Science+Business Media Dordrecht 2014 Abstract We study the velocity dispersion profiles of the NGC 1326 is a ring barred S0 galaxy in the Fornax clus- nuclei of NGC 1326, 2685, 5273 and 5838 in the CO first ter with circumnuclear star formation (Buta et al. 2000). Our overtone band. There is evidence for a black hole (BH) in second galaxy is a Hubble Atlas polar ring galaxy, an S0 NGC 1326 and 5838. Gas is seen flowing out of the nuclear Seyfert 2. Schinnerer and Scoville (2002) detected four giant region of NGC 5273. We put upper limits on the nuclear molecular cloud associations within the polar ring in NGC BHs responsible for its activity and that of NGC 2685. 2685 (the Helix) with of order 107 M of molecular hy- drogen. Dust has been detected with Spitzer in our third S0 Keywords Infrared: general · Active galactic nuclei · galaxy, NGC 5273, totaling 2.5 × 105 M by Martini et al. Galaxies: elliptical · Radiosources · Black holes (2013). NGC5838 has a nuclear star cluster of 5 × 107 M (Scott and Graham 2013). 1 Introduction 2 Sample and observations Understanding activity in galactic nuclei requires high spa- tial resolution. Kormendy and Richstone (1995) have out- We have drawn our radiogalaxy sample from Brown et al. -
Fourier Dissection of Early-Type Galaxy Bars R
The Astronomical Journal, 132:1859Y1876, 2006 November # 2006. The American Astronomical Society. All rights reserved. Printed in U.S.A. FOURIER DISSECTION OF EARLY-TYPE GALAXY BARS R. Buta,1 E. Laurikainen,2 H. Salo,2 D. L. Block,3 and J. H. Knapen4 Received 2006 May 4; accepted 2006 July 14 ABSTRACT This paper reports on a near-infrared survey of early-type galaxies designed to provide information on bar strengths, bulges, disks, and bar parameters in a statistically well-defined sample of S0YSa galaxies. Early-type galaxies have the advantage that their bars are relatively free of the effects of dust, star formation, and spiral structure that com- plicate bar studies in later type galaxies. We describe the survey and present results on a detailed analysis of the rela- tive Fourier intensity amplitudes of bars in 26 early-type galaxies. We also evaluate the ‘‘symmetry assumption’’ of these amplitudes with radius, used recently for bar-spiral separation in later type galaxies. The results show a wide variety of radial Fourier profiles of bars, ranging from simple symmetric profiles that can be represented in terms of a single Gaussian component to both symmetric and asymmetric profiles that can be represented by two overlapping Gaussian components. More complicated profiles than these are also found, often due to multiple barlike features including extended ovals or lenses. Based on the gravitational bar torque indicator Qb, double-Gaussian bars are stronger on average than single-Gaussian bars, at least for our small sample. We show that published numerical simulations in which the bar transfers a large amount of angular momentum to the halo can account for many of the observed profiles. -
Musical Composition Graduate Portfolio
University of Northern Iowa UNI ScholarWorks Dissertations and Theses @ UNI Student Work 2021 Musical composition graduate portfolio Juan Marulanda University of Northern Iowa Let us know how access to this document benefits ouy Copyright ©2021 Juan Marulanda Follow this and additional works at: https://scholarworks.uni.edu/etd Recommended Citation Marulanda, Juan, "Musical composition graduate portfolio" (2021). Dissertations and Theses @ UNI. 1102. https://scholarworks.uni.edu/etd/1102 This Open Access Thesis is brought to you for free and open access by the Student Work at UNI ScholarWorks. It has been accepted for inclusion in Dissertations and Theses @ UNI by an authorized administrator of UNI ScholarWorks. For more information, please contact [email protected]. Copyright by JUAN MARULANDA 2021 All Rights Reserved MUSICAL COMPOSITION GRADUATE PORTFOLIO An Abstract Submitted in Partial Fulfillment of the Requirements for the Degree Master of Music Juan Marulanda University of Northern Iowa May 2021 This Study By: Juan Carlos Marulanda Entitled: Musical Composition Graduate Portfolio has been approved as meeting the thesis requirement for the Degree of Master of Music: Composition Date Dr. Daniel Swilley, Chair, Recital Committee Date Dr. Michael Conrad, Recital Committee Member Date Dr. Jonathan Schwabe, Recital Committee Member Date Dr. Jennifer Waldron, Dean, Graduate College This Recital Performance By: Juan Marulanda Entitled: Musical Composition Graduate Portfolio has been approved as meeting the thesis requirement for the Degree of Master of Music: Composition Date Dr. Daniel Swilley, Chair, Recital Committee Date Dr. Michael Conrad, Recital Committee Member Date Dr. Jonathan Schwabe, Recital Committee Member Date Dr. Jennifer Waldron, Dean, Graduate College ABSTRACT The musical works included in this portfolio were composed between Fall 2019 and Spring 2021. -
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. -
Astronomers Find First Planet from Another Galaxy (W/ Video) 18 November 2010
Astronomers find first planet from another galaxy (w/ Video) 18 November 2010 even though the star now finds itself within our own galaxy. It is part of the so-called Helmi stream - a group of stars that originally belonged to a dwarf galaxy that was devoured by our galaxy, the Milky Way, in an act of galactic cannibalism about six to nine billion years ago. The results are published today in Science Express. "This discovery is very exciting," says Rainer Klement of the Max-Planck-Institut für Astronomie (MPIA), who was responsible for the selection of the target stars for this study. "For the first time, astronomers have detected a planetary system in a stellar stream of extragalactic origin. Because of the great distances involved, there are no This artist’s impression shows HIP 13044 b, an confirmed detections of planets in other galaxies. exoplanet orbiting a star that entered our galaxy, the But this cosmic merger has brought an Milky Way, from another galaxy. This planet of extragalactic planet within our reach." extragalactic origin was detected by a European team of astronomers using the MPG/ESO 2.2-metre telescope at The star is known as HIP 13044, and it lies about ESO’s La Silla Observatory in Chile. The Jupiter-like 2000 light-years from Earth in the southern planet is particularly unusual, as it is orbiting a star nearing the end of its life and could be about to be constellation of Fornax (the Furnace). The engulfed by it, giving clues about the fate of our own astronomers detected the planet, called HIP 13044 planetary system in the distant future. -
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. -
August 13 2016 7:00Pm at the Herrett Center for Arts & Science College of Southern Idaho
Snake River Skies The Newsletter of the Magic Valley Astronomical Society www.mvastro.org Membership Meeting President’s Message Saturday, August 13th 2016 7:00pm at the Herrett Center for Arts & Science College of Southern Idaho. Public Star Party Follows at the Colleagues, Centennial Observatory Club Officers It's that time of year: The City of Rocks Star Party. Set for Friday, Aug. 5th, and Saturday, Aug. 6th, the event is the gem of the MVAS year. As we've done every Robert Mayer, President year, we will hold solar viewing at the Smoky Mountain Campground, followed by a [email protected] potluck there at the campground. Again, MVAS will provide the main course and 208-312-1203 beverages. Paul McClain, Vice President After the potluck, the party moves over to the corral by the bunkhouse over at [email protected] Castle Rocks, with deep sky viewing beginning sometime after 9 p.m. This is a chance to dig into some of the darkest skies in the west. Gary Leavitt, Secretary [email protected] Some members have already reserved campsites, but for those who are thinking of 208-731-7476 dropping by at the last minute, we have room for you at the bunkhouse, and would love to have to come by. Jim Tubbs, Treasurer / ALCOR [email protected] The following Saturday will be the regular MVAS meeting. Please check E-mail or 208-404-2999 Facebook for updates on our guest speaker that day. David Olsen, Newsletter Editor Until then, clear views, [email protected] Robert Mayer Rick Widmer, Webmaster [email protected] Magic Valley Astronomical Society is a member of the Astronomical League M-51 imaged by Rick Widmer & Ken Thomason Herrett Telescope Shotwell Camera https://herrett.csi.edu/astronomy/observatory/City_of_Rocks_Star_Party_2016.asp Calendars for August Sun Mon Tue Wed Thu Fri Sat 1 2 3 4 5 6 New Moon City Rocks City Rocks Lunation 1158 Castle Rocks Castle Rocks Star Party Star Party Almo, ID Almo, ID 7 8 9 10 11 12 13 MVAS General Mtg. -
Gaia Data Release 2: First Stellar Parameters from Apsis
Astronomy & Astrophysics manuscript no. GDR2_Apsis c ESO 2018 3 April 2018 Gaia Data Release 2: first stellar parameters from Apsis René Andrae1, Morgan Fouesneau1, Orlagh Creevey2, Christophe Ordenovic2, Nicolas Mary3, Alexandru Burlacu4, Laurence Chaoul5, Anne Jean-Antoine-Piccolo5, Georges Kordopatis2, Andreas Korn6, Yveline Lebreton7; 8, Chantal Panem5, Bernard Pichon2, Frederic Thévenin2, Gavin Walmsley5, Coryn A.L. Bailer-Jones1? 1 Max Planck Institute for Astronomy, Königstuhl 17, 69117 Heidelberg, Germany 2 Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange, Bd de l’Observatoire, CS 34229, 06304 Nice cedex 4, France 3 Thales Services, 290 Allée du Lac, 31670 Labège, France 4 Telespazio France, 26 Avenue Jean-François Champollion, 31100 Toulouse, France 5 Centre National d’Etudes Spatiales, 18 av Edouard Belin, 31401 Toulouse, France 6 Division of Astronomy and Space Physics, Department of Physics and Astronomy, Uppsala University, Box 516, 75120 Uppsala, Sweden 7 LESIA, Observatoire de Paris, PSL Research University, CNRS UMR 8109, Université Pierre et Marie Curie, Université Paris Diderot, 5 place Jules Janssen, 92190 Meudon 8 Institut de Physique de Rennes, Université de Rennes 1, CNRS UMR 6251, F-35042 Rennes, France Submitted to A&A 21 December 2017. Resubmitted 3 March 2018 and 3 April 2018. Accepted 3 April 2018 ABSTRACT The second Gaia data release (Gaia DR2) contains, beyond the astrometry, three-band photometry for 1.38 billion sources. One band is the G band, the other two were obtained by integrating the Gaia prism spectra (BP and RP). We have used these three broad photometric bands to infer stellar effective temperatures, Teff , for all sources brighter than G = 17 mag with Teff in the range 3 000– 10 000 K (some 161 million sources). -
Public HARPS Radial Velocity Database Corrected for Systematic
A&A 636, A74 (2020) Astronomy https://doi.org/10.1051/0004-6361/201936686 & c T. Trifonov et al. 2020 Astrophysics Public HARPS radial velocity database corrected for systematic errors?,?? Trifon Trifonov1,2, Lev Tal-Or3,4, Mathias Zechmeister5, Adrian Kaminski6, Shay Zucker4, and Tsevi Mazeh7 1 Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany e-mail: [email protected] 2 Department of Astronomy, Sofia University “St Kliment Ohridski”, 5 James Bourchier Blvd, 1164 Sofia, Bulgaria 3 Department of Physics, Ariel University, Ariel 40700, Israel 4 Department of Geophysics, Raymond and Beverly Sackler Faculty of Exact Sciences, Tel Aviv University, Tel Aviv 6997801, Israel 5 Institut für Astrophysik, Georg-August-Universität, Friedrich-Hund-Platz 1, 37077 Göttingen, Germany 6 Landessternwarte, Zentrum für Astronomie der Universtät Heidelberg, Königstuhl 12, 69117 Heidelberg, Germany 7 School of Physics and Astronomy, Raymond and Beverly Sackler Faculty of Exact Sciences, Tel Aviv University, Tel Aviv 6997801, Israel Received 11 September 2019 / Accepted 16 January 2020 ABSTRACT Context. The High Accuracy Radial velocity Planet Searcher (HARPS) spectrograph has been mounted since 2003 at the ESO 3.6 m telescope in La Silla and provides state-of-the-art stellar radial velocity (RV) measurements with a precision down to ∼1 m s−1. The spectra are extracted with a dedicated data-reduction software (DRS), and the RVs are computed by cross-correlating with a numerical mask. Aims. This study has three main aims: (i) Create easy access to the public HARPS RV data set. (ii) Apply the new public SpEctrum Radial Velocity AnaLyser (SERVAL) pipeline to the spectra, and produce a more precise RV data set. -
Does the Fornax Dwarf Spheroidal Have a Central Cusp Or Core?
Research Collection Journal Article Does the Fornax dwarf spheroidal have a central cusp or core? Author(s): Goerdt, Tobias; Moore, Ben; Read, J.I.; Stadel, Joachim; Zemp, Marcel Publication Date: 2006-05 Permanent Link: https://doi.org/10.3929/ethz-b-000024289 Originally published in: Monthly Notices of the Royal Astronomical Society 368(3), http://doi.org/10.1111/ j.1365-2966.2006.10182.x Rights / License: In Copyright - Non-Commercial Use Permitted This page was generated automatically upon download from the ETH Zurich Research Collection. For more information please consult the Terms of use. ETH Library Mon. Not. R. Astron. Soc. 368, 1073–1077 (2006) doi:10.1111/j.1365-2966.2006.10182.x Does the Fornax dwarf spheroidal have a central cusp or core? , Tobias Goerdt,1 Ben Moore,1 J. I. Read,1 Joachim Stadel1 and Marcel Zemp1 2 1Institute for Theoretical Physics, University of Zurich,¨ Winterthurerstrasse 190, CH-8057 Zurich,¨ Switzerland 2Institute of Astronomy, ETH Zurich,¨ ETH Honggerberg¨ HPF D6, CH-8093 Zurich,¨ Switzerland Accepted 2006 February 8. Received 2006 February 7; in original form 2005 December 21 ABSTRACT The dark matter dominated Fornax dwarf spheroidal has five globular clusters orbiting at ∼1 kpc from its centre. In a cuspy cold dark matter halo the globulars would sink to the centre from their current positions within a few Gyr, presenting a puzzle as to why they survive undigested at the present epoch. We show that a solution to this timing problem is to adopt a cored dark matter halo. We use numerical simulations and analytic calculations to show that, under these conditions, the sinking time becomes many Hubble times; the globulars effectively stall at the dark matter core radius. -
Arxiv:1709.05344V1 [Astro-Ph.SR] 15 Sep 2017 (A(Li) = 2.75), Higher Than Its Companion by 0.5 Dex
Draft version September 19, 2017 Typeset using LATEX modern style in AASTeX61 KRONOS & KRIOS: EVIDENCE FOR ACCRETION OF A MASSIVE, ROCKY PLANETARY SYSTEM IN A COMOVING PAIR OF SOLAR-TYPE STARS Semyeong Oh,1, 2 Adrian M. Price-Whelan,1 John M. Brewer,3, 4 David W. Hogg,5, 6, 7, 8 David N. Spergel,1, 5 and Justin Myles3 1Department of Astrophysical Sciences, Princeton University, 4 Ivy Lane, Princeton, NJ 08544, USA 2To whom correspondence should be addressed: [email protected] 3Department of Astronomy, Yale University, 260 Whitney Ave, New Haven, CT 06511, USA 4Department of Astronomy, Columbia University, 550 West 120th Street, New York, NY 10027, USA 5Center for Computational Astrophysics, Flatiron Institute, 162 Fifth Ave, New York, NY 10010, USA 6Center for Cosmology and Particle Physics, Department of Physics, New York University, 726 Broadway, New York, NY 10003, USA 7Center for Data Science, New York University, 60 Fifth Ave, New York, NY 10011, USA 8Max-Planck-Institut f¨ur Astronomie, K¨onigstuhl17, D-69117 Heidelberg ABSTRACT We report and discuss the discovery of a comoving pair of bright solar-type stars, HD 240430 and HD 240429, with a significant difference in their chemical abundances. The two stars have an estimated 3D separation of ≈ 0:6 pc (≈ 0:01 pc projected) at a distance of r ≈ 100 pc with nearly identical three-dimensional velocities, as inferred from Gaia TGAS parallaxes and proper motions, and high-precision radial velocity measurements. Stellar parameters determined from high-resolution Keck HIRES spectra indicate that both stars are ∼ 4 Gyr old. The more metal-rich of the two, HD 240430, shows an enhancement of refractory (TC > 1200 K) elements by ≈ 0:2 dex and a marginal enhancement of (moderately) volatile elements (TC < 1200 K; C, N, O, Na, and Mn). -
Habitability of Planets on Eccentric Orbits: Limits of the Mean Flux Approximation
A&A 591, A106 (2016) Astronomy DOI: 10.1051/0004-6361/201628073 & c ESO 2016 Astrophysics Habitability of planets on eccentric orbits: Limits of the mean flux approximation Emeline Bolmont1, Anne-Sophie Libert1, Jeremy Leconte2; 3; 4, and Franck Selsis5; 6 1 NaXys, Department of Mathematics, University of Namur, 8 Rempart de la Vierge, 5000 Namur, Belgium e-mail: [email protected] 2 Canadian Institute for Theoretical Astrophysics, 60st St George Street, University of Toronto, Toronto, ON, M5S3H8, Canada 3 Banting Fellow 4 Center for Planetary Sciences, Department of Physical & Environmental Sciences, University of Toronto Scarborough, Toronto, ON, M1C 1A4, Canada 5 Univ. Bordeaux, LAB, UMR 5804, 33270 Floirac, France 6 CNRS, LAB, UMR 5804, 33270 Floirac, France Received 4 January 2016 / Accepted 28 April 2016 ABSTRACT Unlike the Earth, which has a small orbital eccentricity, some exoplanets discovered in the insolation habitable zone (HZ) have high orbital eccentricities (e.g., up to an eccentricity of ∼0.97 for HD 20782 b). This raises the question of whether these planets have surface conditions favorable to liquid water. In order to assess the habitability of an eccentric planet, the mean flux approximation is often used. It states that a planet on an eccentric orbit is called habitable if it receives on average a flux compatible with the presence of surface liquid water. However, because the planets experience important insolation variations over one orbit and even spend some time outside the HZ for high eccentricities, the question of their habitability might not be as straightforward. We performed a set of simulations using the global climate model LMDZ to explore the limits of the mean flux approximation when varying the luminosity of the host star and the eccentricity of the planet.