Photographic Catalogue of Deep Sky Objects in Canes Venatici
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Stellar Tidal Streams As Cosmological Diagnostics: Comparing Data and Simulations at Low Galactic Scales
RUPRECHT-KARLS-UNIVERSITÄT HEIDELBERG DOCTORAL THESIS Stellar Tidal Streams as Cosmological Diagnostics: Comparing data and simulations at low galactic scales Author: Referees: Gustavo MORALES Prof. Dr. Eva K. GREBEL Prof. Dr. Volker SPRINGEL Astronomisches Rechen-Institut Heidelberg Graduate School of Fundamental Physics Department of Physics and Astronomy 14th May, 2018 ii DISSERTATION submitted to the Combined Faculties of the Natural Sciences and Mathematics of the Ruperto-Carola-University of Heidelberg, Germany for the degree of DOCTOR OF NATURAL SCIENCES Put forward by GUSTAVO MORALES born in Copiapo ORAL EXAMINATION ON JULY 26, 2018 iii Stellar Tidal Streams as Cosmological Diagnostics: Comparing data and simulations at low galactic scales Referees: Prof. Dr. Eva K. GREBEL Prof. Dr. Volker SPRINGEL iv NOTE: Some parts of the written contents of this thesis have been adapted from a paper submitted as a co-authored scientific publication to the Astronomy & Astrophysics Journal: Morales et al. (2018). v NOTE: Some parts of this thesis have been adapted from a paper accepted for publi- cation in the Astronomy & Astrophysics Journal: Morales, G. et al. (2018). “Systematic search for tidal features around nearby galaxies: I. Enhanced SDSS imaging of the Local Volume". arXiv:1804.03330. DOI: 10.1051/0004-6361/201732271 vii Abstract In hierarchical models of galaxy formation, stellar tidal streams are expected around most galaxies. Although these features may provide useful diagnostics of the LCDM model, their observational properties remain poorly constrained. Statistical analysis of the counts and properties of such features is of interest for a direct comparison against results from numeri- cal simulations. In this work, we aim to study systematically the frequency of occurrence and other observational properties of tidal features around nearby galaxies. -
Star Dust National Capital Astronomers, Inc
Star Dust National Capital Astronomers, Inc. April 10, 2010 Volume 68, Issue 8 http://capitalastronomers.org Next Meeting April 2010: Dr. David J. Thompson When: Sat. Apr. 10, 2010 NASA Goddard Space Flight Center Deputy Project Scientist Time: 7:30 pm Fermi Gamma-ray Space Telescope Where: UM Observatory Highlights from the Fermi Speaker: David Thompson, Gamma-ray Space Telescope NASA Goddard Abstract: Since August, 2008, the Fermi Gamma-ray Space Telescope has Table of Contents been scanning the sky, producing a full-sky image every three hours. The Preview of Apr. 2010 Talk 1 cosmic gamma-rays recorded by Fermi come from extreme astrophysical Spectacular Spiral 2 phenomena. Some key observations include: Octavia Occultation 3 (1) Gamma-rays from pulsars appear to come from a region well above Occultations 4 the surface of the neutron star; Arlington Planetarium 5 (2) Multiwavelength studies of blazars show that simple models of jet Calendar 5 emission are not always adequate to explain what is seen; (3) Gamma-ray bursts can exhibit strong emission at high energies even from Directions to Dinner/Meeting distant bursts, with implications for some models of quantum gravity; Members and guests are invited to (4) Cosmic-ray electrons at energies approaching 1 TeV seem to suggest join us for dinner at the Garden a local source for some of these particles. Restaurant located in the UMUC Inn & Conference Center, 3501 Biography: Dave Thompson University Blvd E. The meeting is received his PhD in physics held at the UM Astronomy from the University of Maryland Observatory on Metzerott Rd about in 1973 and almost immediately started a job at NASA Goddard halfway between Adelphi Rd and Space Flight Center with the University Blvd. -
The Metallicity-Luminosity Relationship of Dwarf Irregular Galaxies
A&A 399, 63–76 (2003) Astronomy DOI: 10.1051/0004-6361:20021748 & c ESO 2003 Astrophysics The metallicity-luminosity relationship of dwarf irregular galaxies II. A new approach A. M. Hidalgo-G´amez1,,F.J.S´anchez-Salcedo2, and K. Olofsson1 1 Astronomiska observatoriet, Box 515, 751 20 Uppsala, Sweden e-mail: [email protected], [email protected] 2 Instituto de Astronom´ıa-UNAM, Ciudad Universitaria, Apt. Postal 70 264, C.P. 04510, Mexico City, Mexico e-mail: [email protected] Received 21 June 2001 / Accepted 21 November 2002 Abstract. The nature of a possible correlation between metallicity and luminosity for dwarf irregular galaxies, including those with the highest luminosities, has been explored using simple chemical evolutionary models. Our models depend on a set of free parameters in order to include infall and outflows of gas and covering a broad variety of physical situations. Given a fixed set of parameters, a non-linear correlation between the oxygen abundance and the luminosity may be established. This would be the case if an effective self–regulating mechanism between the accretion of mass and the wind energized by the star formation could lead to the same parameters for all the dwarf irregular galaxies. In the case that these parameters were distributed in a random manner from galaxy to galaxy, a significant scatter in the metallicity–luminosity diagram is expected. Comparing with observations, we show that only variations of the stellar mass–to–light ratio are sufficient to explain the observed scattering and, therefore, the action of a mechanism of self–regulation cannot be ruled out. -
Flat Galaxy - Above 30 Deg
Flat Galaxy - Above 30 Deg. DEC A B C D E F G H I J K L 1 Const. Object ID Other ID RA Dec Size (arcmin) Mag Urano. Urano. Millennium Notes 2 RFGC NGC hh mm ss dd mm ss.s Major Minor 1st Ed. 2nd Ed. 3 CVn 2245 NGC 4244 12 17 30 +37 48 31 19.4 2.1 10.2 107 54 633 Vol II Note: 4 Com 2335 NGC 4565 12 36 21 +25 59 06 15.9 1.9 10.6 149 71 677 Vol II Note: Slightly asymmetric dust lane 5 Dra 2946 NGC 5907 15 15 52 +56 19 46 12.8 1.4 11.3 50 22 568 Vol II Note: 6 Vir 2315 NGC 4517 12 32 46 +00 06 53 11.5 1.5 11.3 238 110 773 Vol II Note: Dust spots 7 Vir 2579 NGC 5170 13 29 49 -17 57 57 9.9 1.2 11.8 285 130 842 Vol II Note: Eccentric dust lane 8 UMa 2212 NGC 4157 12 11 05 +50 29 07 7.9 1.1 12.2 47 37 592 Vol II Note: 9 Vir 2449 MCG-3-33-30 13 03 17 -17 25 23 8.0 1.1 12.5 284 130 843 Vol II Note: Four knots in the centre 10 CVn 2495 NGC 5023 13 12 12 +44 02 17 7.3 0.8 12.7 75 37 609 Vol II Note: 11 Hya 2682 IC 4351 13 57 54 -29 18 57 6.1 0.8 12.9 371 148 888 Vol II Note: Dust lane. -
EMISSION-LINE NUCLEI at HUBBLE SPACE TELESCOPE RESOLUTION1 Joseph C
The Astrophysical Journal, 654:125Y137, 2007 January 1 # 2007. The American Astronomical Society. All rights reserved. Printed in U.S.A. THE SURVEY OF NEARBY NUCLEI WITH THE SPACE TELESCOPE IMAGING SPECTROGRAPH: EMISSION-LINE NUCLEI AT HUBBLE SPACE TELESCOPE RESOLUTION1 Joseph C. Shields,2 Hans-Walter Rix,3 Marc Sarzi,4 Aaron J. Barth,5 Alexei V. Filippenko,6 Luis C. Ho,7 Daniel H. McIntosh,8 Gregory Rudnick,9,10 and Wallace L. W. Sargent11 Received 2004 August 14; accepted 2006 September 8 ABSTRACT We present results from a program of optical spectroscopy for 23 nearby galaxies with emission-line nuclei. This investigation takes advantage of the spatial resolution of the Hubble Space Telescope to study the structure and energetics of the central 10Y20 pc, and the resulting data have value for quantifying central black hole masses, star formation histories, and nebular properties. This paper provides a description of the experimental design, and new findings from the study of emission lines. The sample targets span a range of nebular spectroscopic class, from H ii to Seyfert nuclei. This data set and the resulting measurements are unique in terms of the sample size, the range of nebular class, and the investigation of physical scales extending down to parsecs. The line ratios indicative of nebular ionization show only modest variations over order-of-magnitude differences in radius, and demonstrate in a sys- tematic way that geometrical dilution of the radiation field from a central source cannot be assumed as a primary driver of ionization structure. Comparisons between large- and small-aperture measurements for the H ii/LINER tran- sition objects provide a new test that challenges conventional wisdom concerning the composite nature of these systems. -
Prime Focus After Sunset
Highlights of the April Sky. - - - 1st - - - Dusk: Mercury is 10º above the western horizon Prime Focus after sunset. Continues until the 15th. A Publication of the Kalamazoo Astronomical Society - - - 3rd - - - Dawn: Antares is 1º below April 2010 the Moon before sunrise. - - - 6th - - - Last Quarter Moon ThisThis MonthsMonths KAS EventsEvents - - - 11th - - - Dawn: Waning Crescent Moon is 5º above Jupiter. General Meeting: Friday, April 9 @ 7:00 pm th - - - 13 - - - PM: Mars is less than 2º Kalamazoo Area Math & Science Center - See Page 8 for Details from the Beehive Cluster (M44) in Cancer. Continues until the 20th. Observing Session: Saturday, April 10 @ 8:00 pm - - - 14th - - - Saturn & Orion Nebula - Kalamazoo Nature Center New Moon th Observing Session: Saturday, April 17 @ 8:00 pm - - - 15 - - - Dusk: Mercury and a very Saturn & Open Clusters - Kalamazoo Nature Center thin crescent Moon 7º to lower right of Venus. Look low on western horizon. Astronomy Day: Saturday, April 24 @ 10:00 am low on western horizon. Kalamazoo Valley Museum & Fetzer Center - See Page 3 for Details - - - 16st - - - PM: Waxing Crescent Moon is 8º above Venus. PM: Pleiades is 3.5º above the Moon/Mercury pair. InsideInside thethe Newsletter.Newsletter. .. .. - - - 21st - - - First Quarter Moon March Meeting Minutes......................... p. 2 - - - 23rd - - - PM: Venus and Pleiades fit Board Meeting Minutes......................... p. 2 within a 5º field-of-view. Astronomy Day 2010............................ p. 3 - - - 24th - - - Astronomy Day Spectacular Spiral................................... p. 4 PM: Waxing Gibbous Moon NASA Space Place.................................. p. 5 is lower right of Saturn. April Night Sky........................................ p. 6 - - - 25th - - - PM: Waxing Gibbous Moon KAS Officers & Announcements........ p. 7 is lower left of Saturn. -
Machine Learning for Star Cluster Identification∗ Submitted to Apj
Draft version December 1, 2020 Typeset using LATEX default style in AASTeX63 StarcNet: Machine Learning for Star Cluster Identification∗ Gustavo Perez´ ,1 Matteo Messa ,2 Daniela Calzetti ,2 Subhransu Maji ,1 Dooseok E. Jung ,2 Angela Adamo ,3 and Mattia Siressi3 1Department of Computer Science University of Massachusetts Amherst 40 Governors Drive Amherst, MA 01003, USA 2Department of Astronomy University of Massachusetts Amherst 710 North Pleasant Street Amherst, MA 01003, USA 3Department of Astronomy, Oskar Klein Centre, Stockholm University, AlbaNova University Centre, SE-106 91 Stockholm, Sweden (Received July 1, 2020; Revised; Accepted) Submitted to ApJ ABSTRACT We present a machine learning (ML) pipeline to identify star clusters in the multi{color images of nearby galaxies, from observations obtained with the Hubble Space Telescope as part of the Treasury Project LEGUS (Legacy ExtraGalactic Ultraviolet Survey). StarcNet (STAR Cluster classification NETwork) is a multi{scale convolutional neural network (CNN) which achieves an accuracy of 68.6% (4 classes)/86.0% (2 classes: cluster/non{cluster) for star cluster classification in the images of the LEGUS galaxies, nearly matching human expert performance. We test the performance of StarcNet by applying pre{trained CNN model to galaxies not included in the training set, finding accuracies similar to the reference one. We test the effect of StarcNet predictions on the inferred cluster properties by comparing multi{color luminosity functions and mass{age plots from catalogs produced by StarcNet and by human{labeling; distributions in luminosity, color, and physical characteristics of star clusters are similar for the human and ML classified samples. There are two advantages to the ML approach: (1) reproducibility of the classifications: the ML algorithm's biases are fixed and can be measured for subsequent analysis; and (2) speed of classification: the algorithm requires minutes for tasks that humans require weeks to months to perform. -
121012-AAS-221 Program-14-ALL, Page 253 @ Preflight
221ST MEETING OF THE AMERICAN ASTRONOMICAL SOCIETY 6-10 January 2013 LONG BEACH, CALIFORNIA Scientific sessions will be held at the: Long Beach Convention Center 300 E. Ocean Blvd. COUNCIL.......................... 2 Long Beach, CA 90802 AAS Paper Sorters EXHIBITORS..................... 4 Aubra Anthony ATTENDEE Alan Boss SERVICES.......................... 9 Blaise Canzian Joanna Corby SCHEDULE.....................12 Rupert Croft Shantanu Desai SATURDAY.....................28 Rick Fienberg Bernhard Fleck SUNDAY..........................30 Erika Grundstrom Nimish P. Hathi MONDAY........................37 Ann Hornschemeier Suzanne H. Jacoby TUESDAY........................98 Bethany Johns Sebastien Lepine WEDNESDAY.............. 158 Katharina Lodders Kevin Marvel THURSDAY.................. 213 Karen Masters Bryan Miller AUTHOR INDEX ........ 245 Nancy Morrison Judit Ries Michael Rutkowski Allyn Smith Joe Tenn Session Numbering Key 100’s Monday 200’s Tuesday 300’s Wednesday 400’s Thursday Sessions are numbered in the Program Book by day and time. Changes after 27 November 2012 are included only in the online program materials. 1 AAS Officers & Councilors Officers Councilors President (2012-2014) (2009-2012) David J. Helfand Quest Univ. Canada Edward F. Guinan Villanova Univ. [email protected] [email protected] PAST President (2012-2013) Patricia Knezek NOAO/WIYN Observatory Debra Elmegreen Vassar College [email protected] [email protected] Robert Mathieu Univ. of Wisconsin Vice President (2009-2015) [email protected] Paula Szkody University of Washington [email protected] (2011-2014) Bruce Balick Univ. of Washington Vice-President (2010-2013) [email protected] Nicholas B. Suntzeff Texas A&M Univ. suntzeff@aas.org Eileen D. Friel Boston Univ. [email protected] Vice President (2011-2014) Edward B. Churchwell Univ. of Wisconsin Angela Speck Univ. of Missouri [email protected] [email protected] Treasurer (2011-2014) (2012-2015) Hervey (Peter) Stockman STScI Nancy S. -
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. -
Arxiv:0907.4718V1 [Astro-Ph.GA] 27 Jul 2009 Nnab Aais Hi Ihlmnste ( Luminosities High Their Objects Point-Like Galaxies
Submitted to Astrophysical Journal A Preprint typeset using L TEX style emulateapj v. 04/03/99 ULTRALUMINOUS X-RAY SOURCE CORRELATIONS WITH STAR-FORMING REGIONS Douglas A. Swartz1 Allyn F. Tennant2, and Roberto Soria3 Submitted to Astrophysical Journal ABSTRACT Maps of low-inclination nearby galaxies in Sloan Digitized Sky Survey u − g, g − r and r − i colors are used to determine whether Ultraluminous X-ray sources (ULXs) are predominantly associated with star-forming regions of their host galaxies. An empirical selection criterion is derived from colors of H ii regions in M 81 and M 101 that differentiates between the young, blue stellar component and the older disk and bulge population. This criterion is applied to a sample of 58 galaxies of Hubble type S0 and later and verified through an application of Fisher’s linear discriminant analysis. It is found that 60% (49%) of ULXs in optically-bright environments are within regions blueward of their host galaxy’s H ii regions compared to only 27% (0%) of a control sample according to the empirical (Fisher) criterion. This is an excess of 3σ above the 32% (27%) expected if the ULXs were randomly distributed within their galactic hosts. This indicates a ULX preference for young, ∼<10 Myr, OB associations. However, none of the ULX environments have the morphology and optical brightness suggestive of a massive young super star cluster though several are in extended or crowded star-forming (blue) environments that may contain clusters unresolved by Sloan imaging. Ten of the 12 ULX candidates with estimated X-ray luminosities in excess of 3×1039 ergs s−1 are equally divided among the group of ULX environments redward of H ii regions and the group of optically faint regions. -
University of Groningen Warps in Disk Galaxies Garcнa Ruiz, Iсigo
University of Groningen Warps in disk galaxies García Ruiz, Iñigo IMPORTANT NOTE: You are advised to consult the publisher's version (publisher's PDF) if you wish to cite from it. Please check the document version below. Document Version Publisher's PDF, also known as Version of record Publication date: 2001 Link to publication in University of Groningen/UMCG research database Citation for published version (APA): García Ruiz, I. (2001). Warps in disk galaxies. s.n. Copyright Other than for strictly personal use, it is not permitted to download or to forward/distribute the text or part of it without the consent of the author(s) and/or copyright holder(s), unless the work is under an open content license (like Creative Commons). The publication may also be distributed here under the terms of Article 25fa of the Dutch Copyright Act, indicated by the “Taverne” license. More information can be found on the University of Groningen website: https://www.rug.nl/library/open-access/self-archiving-pure/taverne- amendment. Take-down policy If you believe that this document breaches copyright please contact us providing details, and we will remove access to the work immediately and investigate your claim. Downloaded from the University of Groningen/UMCG research database (Pure): http://www.rug.nl/research/portal. For technical reasons the number of authors shown on this cover page is limited to 10 maximum. Download date: 07-10-2021 4 Neutral Hydrogen and Optical Observations of Edge-on Galaxies: The data Based on a paper by I. Garc´ıa-Ruiz, R. Sancisi & K. -
NGC -- IC Messier Type Constellation Mag Dimension Dist Al NGC
NGC -- IC Messier Type Constellation Mag Dimension Dist al NGC 1952 M 001 Vestiges de Supernovæ - Crabe Taureau 8,4 6' x 4' 6300 NGC 7089 M 002 Amas globulaire Verseau 6,5 16' 37500 NGC 5272 M 003 Amas globulaire Chiens de Chasse 6,2 18' 33900 NGC 6121 M 004 Amas globulaire Scorpion 5,6 36' 7200 NGC 5904 M 005 Amas globulaire Serpent 5,6 23' 24500 NGC 6405 M 006 Amas ouvert - Papillon Scorpion 4,2 25' 1589 NGC 6475 M 007 Amas ouvert - Ptolémée Scorpion 3,3 80' 978 NGC 6523 M 008 Nébuleuse diffuse du Lagon Sagittaire 6 90' x 40' 5200 NGC 6333 M 009 Amas globulaire Ophiuchus 7,7 12' 25800 NGC 6234 M 010 Amas globulaire Ophiuchus 6,6 20' 14300 NGC 6705 M 011 Amas ouvert - Canard Sauvage Écu de sobieski 6,3 14' 6122 NGC 6218 M 012 Amas globulaire Ophiuchus 6,7 16' 16000 NGC 6205 M 013 Amas globulaire – Grand amas d'hercul Hercule 5,8 20' 25100 NGC 6402 M 014 Amas globulaire Ophiuchus 7,6 11' 30300 NGC 7078 M 015 Amas globulaire Pégase 6,2 1' 33600 NGC 6611 M 016 Amas ouvert + nébuleuse Serpent 6,4 7' 5607 NGC 6618 M 017 Nébuleuse diffuse - Oméga Sagittaire 6 46' x 36' 5916 NGC 6613 M 018 Amas ouvert Sagittaire 7,5 9' 4227 NGC 6273 M 019 Amas globulaire Ophiuchus 6,8 17' 28000 NGC 6514 M 020 Nébuleuse diffuse - Trifide Sagittaire 6,3 28' 2661 NGC 6531 M 021 Amas ouvert Sagittaire 6,5 13' 3930 NGC 6656 M 022 Amas globulaire Sagittaire 5,1 32' 10400 NGC 6494 M 023 Amas ouvert Sagittaire 6,9 27' 2048 IC 4715 M 024 Nuage galactique Sagittaire 4,6 90' 10000 IC 4725 M 025 Amas ouvert Sagittaire 4,6 32' 2000 NGC 6694 M 026 Amas ouvert Écu de sobieski