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HST/WFPC2 Imaging of the Circumnuclear Structure of Llagns
HST/WFPC2 imaging of the circumnuclear structure of LLAGNs. I Data and nuclear morphology1 Rosa M. Gonz´alez Delgado1, Enrique P´erez1, Roberto Cid Fernandes2, Henrique Schmitt3, (1) Instituto de Astrof´ısica de Andaluc´ıa(CSIC), P.O. Box 3004, 18080 Granada, Spain ([email protected]; [email protected]) (2) Depto. de F´ısica-CFM, Universidade Federal de Santa Catarina, C.P. 476, 88040-900, Florian´opolis, SC, Brazil ([email protected]) (3) Remote Sensing Division, Naval Research Laboratory, Code 7210, 4555 Overlook Avenue, Washington, DC 20375 ([email protected]) (4) Interferometrics, Inc., 13454 Sunrise Valley Drive, Suite 240, Herndon, VA20171 ABSTRACT In several studies of Low Luminosity Active Galactic Nuclei (LLAGNs), we have characterized the properties of the stellar populations in LINERs and LINER/HII Transition Objects (TOs). We have found a numerous class of galac- tic nuclei which stand out because of their conspicuous 0.1–1 Gyr populations. These nuclei were called ”Young-TOs” since they all have TO-like emission line ratios. To advance our knowledge of the nature of the central source in LLAGNs and its relation with stellar clusters, we are carrying out several imaging projects with the Hubble Space Telescope (HST) at near-UV, optical and near-IR wave- lengths. In this paper, we present the first results obtained with observations of the central regions of 57 LLAGNs imaged with the WFPC2 through any of arXiv:0710.4450v1 [astro-ph] 24 Oct 2007 the V (F555W, F547M, F614W) and I (F791W, F814W) filters that are avail- able in the HST archive. -
Nova Report 2006-2007
NOVA REPORTNOVA 2006 - 2007 NOVA REPORT 2006-2007 Illustration on the front cover The cover image shows a composite image of the supernova remnant Cassiopeia A (Cas A). This object is the brightest radio source in the sky, and has been created by a supernova explosion about 330 year ago. The star itself had a mass of around 20 times the mass of the sun, but by the time it exploded it must have lost most of the outer layers. The red and green colors in the image are obtained from a million second observation of Cas A with the Chandra X-ray Observatory. The blue image is obtained with the Very Large Array at a wavelength of 21.7 cm. The emission is caused by very high energy electrons swirling around in a magnetic field. The red image is based on the ratio of line emission of Si XIII over Mg XI, which brings out the bi-polar, jet-like, structure. The green image is the Si XIII line emission itself, showing that most X-ray emission comes from a shell of stellar debris. Faintly visible in green in the center is a point-like source, which is presumably the neutron star, created just prior to the supernova explosion. Image credits: Creation/compilation: Jacco Vink. The data were obtained from: NASA Chandra X-ray observatory and Very Large Array (downloaded from Astronomy Digital Image Library http://adil.ncsa.uiuc. edu). Related scientific publications: Hwang, Vink, et al., 2004, Astrophys. J. 615, L117; Helder and Vink, 2008, Astrophys. J. in press. -
(Ap) Mag Size Distance Rise Transit Set Gal NGC 6217 Arp 185 Umi
Herschel 400 Observing List, evening of 2015 Oct 15 at Cleveland, Ohio Sunset 17:49, Twilight ends 19:18, Twilight begins 05:07, Sunrise 06:36, Moon rise 09:51, Moon set 19:35 Completely dark from 19:35 to 05:07. Waxing Crescent Moon. All times local (EST). Listing All Classes visible above the perfect horizon and in twilight or moonlight before 23:59. Cls Primary ID Alternate ID Con RA (Ap) Dec (Ap) Mag Size Distance Rise Transit Set Gal NGC 6217 Arp 185 UMi 16h31m48.9s +78°10'18" 11.9 2.6'x 2.1' - 15:22 - Gal NGC 2655 Arp 225 Cam 08h57m35.6s +78°09'22" 11 4.5'x 2.8' - 7:46 - Gal NGC 3147 MCG 12-10-25 Dra 10h18m08.0s +73°19'01" 11.3 4.1'x 3.5' - 9:06 - PNe NGC 40 PN G120.0+09.8 Cep 00h13m59.3s +72°36'43" 10.7 1.0' 3700 ly - 23:03 - Gal NGC 2985 MCG 12-10-6 UMa 09h51m42.0s +72°12'01" 11.2 3.8'x 3.1' - 8:39 - Gal Cigar Galaxy M 82 UMa 09h57m06.5s +69°35'59" 9 9.3'x 4.4' 12.0 Mly - 8:45 - Gal NGC 1961 Arp 184 Cam 05h43m51.6s +69°22'44" 11.8 4.1'x 2.9' 180.0 Mly - 4:32 - Gal NGC 2787 MCG 12-9-39 UMa 09h20m40.5s +69°07'51" 11.6 3.2'x 1.8' - 8:09 - Gal NGC 3077 MCG 12-10-17 UMa 10h04m31.3s +68°39'09" 10.6 5.1'x 4.2' 12.0 Mly - 8:52 - Gal NGC 2976 MCG 11-12-25 UMa 09h48m29.2s +67°50'21" 10.8 6.0'x 3.1' 15.0 Mly - 8:36 - PNe Cat's Eye Nebula NGC 6543 Dra 17h58m31.7s +66°38'25" 8.3 22" 4400 ly - 16:49 - Open NGC 7142 Collinder 442 Cep 21h45m34.2s +65°51'16" 10 12.0' 5500 ly - 20:35 - Gal NGC 2403 MCG 11-10-7 Cam 07h38m20.9s +65°33'36" 8.8 20.0'x 10.0' 11.0 Mly - 6:26 - Open NGC 637 Collinder 17 Cas 01h44m15.4s +64°07'07" 7.3 3.0' 7000 ly - 0:33 -
Globular Cluster Systems of Six Shell Galaxies
A&A 458, 53–67 (2006) Astronomy DOI: 10.1051/0004-6361:20054606 & c ESO 2006 Astrophysics Globular cluster systems of six shell galaxies G. Sikkema1,R.F.Peletier1, D. Carter2, E. A. Valentijn1, and M. Balcells3 1 Kapteyn Astronomical Institute, University of Groningen, PO Box 800, 9700 AV Groningen, The Netherlands e-mail: [email protected] 2 Astrophysics Research Institute, Liverpool John Moores University, 12 Quays House, Egerton Wharf, Birkenhead, CH41 1LD, UK 3 Instituto de Astrofísica de Canarias, vía Láctea s/n, La Laguna 38200, Spain Received 29 November 2005 / Accepted 14 June 2006 ABSTRACT Context. Shells in Elliptical Galaxies are faint, sharp-edged features, believed to provide evidence of a recent (∼0.5−2 × 109 years ago) merger event. We analyse the Globular Cluster (GC) systems of six shell elliptical galaxies, to examine the effects of mergers upon the GC formation history. Aims. We examine the colour distributions, and investigate differences between red and blue globular cluster populations. We present luminosity functions, spatial distributions and specific frequencies (SN ) at 50 kpc radius for our sample. Methods. We present V and I magnitudes for cluster candidates measured with the HST Advanced Camera for Surveys (ACS). Galaxy background light is modelled and removed, and magnitudes are measured in 8 pixel (0.4 arcsec) diameter apertures. Background contamination is removed using counts from Hubble Deep Field South. Results. We find that the colour distributions for NGC 3923 and NGC 5982 have a bimodal form typical of bright ellipticals, with peaks near V − I = 0.92 ± 0.04 and V − I = 1.18 ± 0.06. -
STARDUST Newsletter of the Royal Astronomical Society of Canada Edmonton Centre
STARDUST Newsletter of the Royal Astronomical Society of Canada Edmonton Centre May 2011 Volume 57 Issue 9 Maria Vergara of Oliver School stands by her award-winning astronomy display. Details on page 4. Inside this Issue Contact Information................................................................................................................................................page 2 Upcoming Events, Meetings, Deadlines, Announcements.....................................................................................page 3 President's Report....................................................................................................................................................page 3 Best Astronomy Award 2011..................................................................................................................................page 4 Book Donations.......................................................................................................................................................page 4 GA Logo Contest! ..................................................................................................................................................Page 5 Observers Report.....................................................................................................................................................page 5 The Planets..............................................................................................................................................................page 6 Stardust -
Constellation : Dra=Le Dragon Nom Distance (Al) Magnitude Type Spectr
Le Dragon 1 Constellation : Dra=le Dragon Nom distance (al) magnitude type spectr. remarques ααα ou Thuban 200 3,6 M0III βββ ou Alwaïd ou Rastaban 400 2,79 G2Ib γγγ ou Etamin ou Eltanin 150 2,24 K5III δδδ ou Nodus II ou Al Taïs 99 3,07 G9III ννν ou Kuma 100 4,9 et... A6V et.. binaire A: blanche 4,9 A5 B à à 62" ξξξ ou Grumium 200 3,8 K2III ζζζ ou Nodus I ou Adhibah 300 3,17 B6III εεε ou Tyl 146 3,8 et K0III et Etoile double, A : jaune-orange 7 K0 B à 3,4" ιιι ou Edasish ou Ed Asic 100 3.42 et K2IIIet étoile binaire : A : orange 8.87 K7 B à 4'14" A possède 1 planète extrasolaire b : m=8,6MJup. p=550j. d=1,34ua) λλλ ou Gianfar ou Giauzar 125 4,1 M0III ΦΦΦ 270 4,2 A0 Le Dragon 2 σσσ ou ΑΑΑl safi 18 4,7 K0V µµµ ou Arrabis 88 5.66 et F7Vet Binaire A jaune 5.69 F5 B à 2,3" de période 482 ans ψψψ1ψ1 ou Dsiban 72 4,6 et F5IV et binaire A : blanche 5,6 F8 B à 30" ψψψ2ψ222 720 5,4 F2II ηηη 88 2,73 G8III étoile triple (difficile à voir) θθθ 64 4,1 F8IV κκκ 400 3,9 B6III οοο 320 4,6 et G9III Etoile double A : orange 8,2 B : rouge-orange. à 37" Etoile triple liée. 17 et 398 5.38 et B9V 17 A bleue 6.42 A2 B à 3.2" 16 5.50 B9V 16 à 1'29" de 17 39 189 5 et A4 et Etoile triple, A : blanche 7,9 et F8 et B : à 1'30"de A 7,5 A2 C à 3,7" de A Etoile triple 41 et 173 5,74 K2V 41 A : jaune et variable 5,7 F5 B A 18" 40 166 F7 .40 à 3'44" de 41 La Petite Reine un objet STAR d'Harrington , (Little Queen), astérisme ayant la forme d'un W, comme la Grande Reine : Cassiopée. -
Astronomy Magazine 2020 Index
Astronomy Magazine 2020 Index SUBJECT A AAVSO (American Association of Variable Star Observers), Spectroscopic Database (AVSpec), 2:15 Abell 21 (Medusa Nebula), 2:56, 59 Abell 85 (galaxy), 4:11 Abell 2384 (galaxy cluster), 9:12 Abell 3574 (galaxy cluster), 6:73 active galactic nuclei (AGNs). See black holes Aerojet Rocketdyne, 9:7 airglow, 6:73 al-Amal spaceprobe, 11:9 Aldebaran (Alpha Tauri) (star), binocular observation of, 1:62 Alnasl (Gamma Sagittarii) (optical double star), 8:68 Alpha Canum Venaticorum (Cor Caroli) (star), 4:66 Alpha Centauri A (star), 7:34–35 Alpha Centauri B (star), 7:34–35 Alpha Centauri (star system), 7:34 Alpha Orionis. See Betelgeuse (Alpha Orionis) Alpha Scorpii (Antares) (star), 7:68, 10:11 Alpha Tauri (Aldebaran) (star), binocular observation of, 1:62 amateur astronomy AAVSO Spectroscopic Database (AVSpec), 2:15 beginner’s guides, 3:66, 12:58 brown dwarfs discovered by citizen scientists, 12:13 discovery and observation of exoplanets, 6:54–57 mindful observation, 11:14 Planetary Society awards, 5:13 satellite tracking, 2:62 women in astronomy clubs, 8:66, 9:64 Amateur Telescope Makers of Boston (ATMoB), 8:66 American Association of Variable Star Observers (AAVSO), Spectroscopic Database (AVSpec), 2:15 Andromeda Galaxy (M31) binocular observations of, 12:60 consumption of dwarf galaxies, 2:11 images of, 3:72, 6:31 satellite galaxies, 11:62 Antares (Alpha Scorpii) (star), 7:68, 10:11 Antennae galaxies (NGC 4038 and NGC 4039), 3:28 Apollo missions commemorative postage stamps, 11:54–55 extravehicular activity -
Astronomy and Astrophysics Research Report 2008
Astronomy and Astrophysics Research Report 2008 Adopted by the Governing Board of the School of Cosmic Physics on 4th March 2009 Contents 1 Highlights 4 2 Staff 5 3 Research Reports 6 3.1 Brown Dwarf Outflow Studies . 6 3.2 First Detection of an Atomic Jet from an Embedded Protostar . 6 3.3 Detailed observational studies of stellar outflows . 6 3.4 Automatic Pipeline from Jet Simulations to Synthetic Observations . 7 3.5 MHD models for jets . 7 3.6 High Resolution Spectroscopy of Brown Dwarfs . 8 3.7 Ultra-precise photometry from space . 8 3.8 Kuiper-Belt objects . 8 3.9 Shells in elliptical galaxies . 9 3.10 An ACS Treasury survey of the Coma Cluster . 9 3.11 La Palma International Time Programme: Fossil groups . 9 3.12 Interstellar medium of the Milky Way . 9 3.13 Formation of Structure in Low-Beta Regions of the ISM . 10 3.14 MHD Simulations of Star-forming Regions . 10 3.15 Radiative Effects in the Interstellar Medium . 11 3.16 Simulated Polarimetric Observations of Stellar Jets . 11 3.17 Computational studies of ISM turbulence . 11 3.18 Gamma Ray Bursts: REM Telescope observations . 12 3.19 High resolution echelle spectroscopy of GRB afterglows . 13 3.20 Echelle spectroscopy of runaway stars . 14 3.21 OB runaway star lightcurves . 15 3.22 High-energy emission from young stellar clusters . 16 3.23 High-energy sources in galaxies . 17 1 3.24 Supernova candidates in the solar neighbourhood . 17 3.25 AGN contributions to HDF galaxies . 17 3.26 X-ray observations of the 2007 PSR B1259-63 periastron passage . -
Radio Sources in Low-Luminosity Active Galactic Nuclei
A&A 435, 521–543 (2005) Astronomy DOI: 10.1051/0004-6361:20042277 & c ESO 2005 Astrophysics Radio sources in low-luminosity active galactic nuclei IV. Radio luminosity function, importance of jet power, and radio properties of the complete Palomar sample N. M. Nagar1,2, H. Falcke3, and A. S. Wilson4 1 Kapteyn Institute, Landleven 12, 9747 AD Groningen, The Netherlands 2 Astronomy Group, Departamento de Física, Universidad de Concepción, Casilla 160-C, Concepción, Chile e-mail: [email protected] 3 ASTRON, PO Box 2, 7990 AA Dwingeloo, The Netherlands Department of Astronomy, Radboud University Nijmegen, Postbus 9010, 6500 GL Nijmegen, The Netherlands e-mail: [email protected] 4 Department of Astronomy, University of Maryland, College Park, MD 20742, USA Adjunct Astronomer, Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA e-mail: [email protected] Received 29 October 2004 / Accepted 5 February 2005 Abstract. We present the completed results of a high resolution radio imaging survey of all (∼200) low-luminosity active galactic nuclei (LLAGNs) and AGNs in the Palomar Spectroscopic Sample of all (∼488) bright northern galaxies. The high incidences of pc-scale radio nuclei, with implied brightness temperatures ∼>107 K, and sub-parsec jets argue for accreting black holes in ∼>50% of all LINERs and low-luminosity Seyferts; there is no evidence against all LLAGNs being mini-AGNs. The detected parsec-scale radio nuclei are preferentially found in massive ellipticals and in type 1 nuclei (i.e. nuclei with broad Hα emission). The radio luminosity function (RLF) of Palomar Sample LLAGNs and AGNs extends three orders of magnitude below, and is continuous with, that of “classical” AGNs. -
Elliptical Galaxies: Structure, Stellar Content, and Evolution
Elliptical Galaxies: Structure, Stellar Content, and Evolution Thesis by Michael Andrew Pahre In Partial Ful¯llment of the Requirements for the Degree of Doctor of Philosophy California Institute of Technology Pasadena, California 1998 (Submitted February 3, 1998) ii c 1998 ° Michael Andrew Pahre All Rights Reserved iii Abstract A near{infrared imaging survey of 341 nearby early{type galaxies, combined with optical imaging and spectroscopic data from the literature, are used to construct the global scaling relations for this population of galaxies. These data demonstrate a number of important features of the early{type galaxy sequence: (1) the slope of the Fundamental Plane (FP) correlations systematically increases with wavelength; (2) the slope of these FP correlations deviates from the virial expectation at all wavelengths, implying a breakdown of either or both of the assumptions of constant mass{to{light ratio and homology; (3) the intrinsic scatter of the FP correlations is small but resolved at all wavelengths, implying a small cosmic scatter of early{type galaxy properties at any position in the galaxy sequence and contradicting any model in which various stellar populations parameters \conspire" with each other to keep the correlations thin at optical wavelengths; (4) there is no correla- tion among residuals of the metallicity{independent near{infrared FP and the metallicity{ sensitive Mg2{σ0 relation, implying that both age and metallicity variations contribute to the cosmic scatter of both correlations; and (5) the e®ective radii systematically decrease with increasing wavelength, fully consistent with the general presence of stellar populations gradients in early{type galaxies. A comprehensive and self{consistent model is described which simultaneously explains these and other global properties of the early{type galaxy sequence. -
In This Issue: Appointment As the Inaugural Baruch S
The Rosette Gazette Volume 26,, IssueIssue 7 Newsletter of the Rose City Astronomers July, 2013 The Human Role in Earth Evolution David Grinspoon From the perspective of Astrobiology, David will review Earth history and offer a taxonomy of catastrophe that examines the changing roles of life and so-called intelligence in our evolving planet, and implications for the prospect of advanced life elsewhere in the universe. Bio: David Grinspoon is an astrobiologist who studies the possible conditions for life on other planets. In November 2012, he began a one-year In This Issue: appointment as the inaugural Baruch S. Blumberg/NASA Chair in Astrobiology at the John W. Kluge Center of the United States Library of 1….General Meeting Congress, where he is researching and writing a book about the human 2….Club Contacts influence on Earth, seen in cosmic perspective. He is Curator of Astrobiology at the Denver Museum of Nature & Science, and Adjunct 3.....RCA Board Minutes Professor of Astrophysical and Planetary Science at the University of Colorado. He is a frequent advisor to NASA on space exploration strategy, and is Co-Investigator on an 4….Special Interest instrument that is currently operating on the Curiosity Rover on Mars. He serves as Interdisciplinary Groups Scientist on the European Space Agency’s Venus Express spacecraft, which is currently in orbit around Venus. Grinspoon was awarded the 2006 Carl Sagan Medal for Public Communication of Planetary 5.....A Treasury of Science by the American Astronomical Society. His first book, Venus Revealed, was a Los Angeles Vintage Eyepieces Times Book Prize finalist. -
Dave Mitsky's Monthly Celestial Calendar
Dave Mitsky’s Monthly Celestial Calendar January 2010 ( between 4:00 and 6:00 hours of right ascension ) One hundred and five binary and multiple stars for January: Omega Aurigae, 5 Aurigae, Struve 644, 14 Aurigae, Struve 698, Struve 718, 26 Aurigae, Struve 764, Struve 796, Struve 811, Theta Aurigae (Auriga); Struve 485, 1 Camelopardalis, Struve 587, Beta Camelopardalis, 11 & 12 Camelopardalis, Struve 638, Struve 677, 29 Camelopardalis, Struve 780 (Camelopardalis); h3628, Struve 560, Struve 570, Struve 571, Struve 576, 55 Eridani, Struve 596, Struve 631, Struve 636, 66 Eridani, Struve 649 (Eridanus); Kappa Leporis, South 473, South 476, h3750, h3752, h3759, Beta Leporis, Alpha Leporis, h3780, Lallande 1, h3788, Gamma Leporis (Lepus); Struve 627, Struve 630, Struve 652, Phi Orionis, Otto Struve 517, Beta Orionis (Rigel), Struve 664, Tau Orionis, Burnham 189, h697, Struve 701, Eta Orionis, h2268, 31 Orionis, 33 Orionis, Delta Orionis (Mintaka), Struve 734, Struve 747, Lambda Orionis, Theta-1 Orionis (the Trapezium), Theta-2 Orionis, Iota Orionis, Struve 750, Struve 754, Sigma Orionis, Zeta Orionis (Alnitak), Struve 790, 52 Orionis, Struve 816, 59 Orionis, 60 Orionis (Orion); Struve 476, Espin 878, Struve 521, Struve 533, 56 Persei, Struve 552, 57 Persei (Perseus); Struve 479, Otto Struve 70, Struve 495, Otto Struve 72, Struve 510, 47 Tauri, Struve 517, Struve 523, Phi Tauri, Burnham 87, Xi Tauri, 62 Tauri, Kappa & 67 Tauri, Struve 548, Otto Struve 84, Struve 562, 88 Tauri, Struve 572, Tau Tauri, Struve 598, Struve 623, Struve 645, Struve