Interpretation of the Stephan Quintet Galaxy Cluster Using Hydro-Gravitational Theory
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History Committee Report NC185: Robotic Telescope— Page | 1 Suggested Celestial Targets with Historical Canadian Resonance
RASC History Committee Report NC185: Robotic Telescope— Page | 1 Suggested Celestial Targets with Historical Canadian Resonance 2018 September 16 Robotic Telescope—Suggested Celestial Targets with Historical Canadian Resonance ABSTRACT: At the request of the Society’s Robotic Telescope Team, the RASC History Committee has compiled a list of over thirty (30) suggested targets for imaging with the RC Optical System (Ritchey- Chrétien f/9 0.4-metre class, with auxiliary wide-field capabilities), chosen from mainly “deep sky objects Page | 2 which are significant in that they are linked to specific events or people who were noteworthy in the 150 years of Canadian history”. In each numbered section the information is arranged by type of object, with specific targets suggested, the name or names of the astronomers (in bold) the RASC Robotic Telescope image is intended to honour, and references to select relevant supporting literature. The emphasis throughout is on Canadian astronomers (in a generous sense), and RASC connections. NOTE: The nature of Canadian observational astronomy over most of that time changed slowly, but change it did, and the accepted celestial targets, instrumental capabilities, and recording methods are frequently different now than they were in 1868, 1918, or 1968, and those differences can startle those with modern expectations looking for analogues to present/contemporary practice. The following list attempts to balance those expectations, as well as the commemoration of professionals and amateurs from our past. 1. OBJECT: Detail of lunar terminator (any feature). ACKNOWLEDGES: 18th-19th century practical astronomy (astronomy of place & time), the practitioners of which used lunar observation (shooting lunars) to determine longitude. -
VV Compact Groups of Galaxies&Q
PRINCETON UNIVERSITY Department of Astrophysical Sciences Final Report for grant UAG-8363 "V-V Compact Groups of Galaxies" for National Aeronautics and Space Administration Marshall Space Flight Center By: Neta A. Bahcall Principal Investigator June 1984 X-ray Emission from Stephen's Quintet and Other Compact Groups by Neta A. Bahcall Space Telescope Science Institute D. E. Harris High Energy Astrophysics, Center for Astrophysics Herbert J. Rood Box 1330, Princeton, NJ 08542 Abstract A search for X-ray emission from five compact groups of galaxies with the Einstein Observatory revealed detections from three groups. Soft, extended X- ray emission was observed in Stephen's Quintet which is most likely caused by hot intracluster gas. This provides evidence for dynamical interaction among the group galaxies. X-ray emission from the group Arp 330 may also originate in hot intracluster gas. Stephen's Quintet and Arp 330 have the largest velocity dispersions among the groups studied suggesting a correlation between high velocity and the release (or properties) of hot gas. X-ray emission from Arp 318 may originate in its member galaxies. I. Introduction The X-ray emission detected from rich clusters of galaxies reveals a hot metal-enriched intracluster medium (ICM) that probably originated from processed gas swept-out of galaxies. This provides direct evidence for the occurrence of interactions among cluster galaxies. Since dynamical interactions depend on the galaxy (and/or ICM) density, they are expected to be important in the groups of highest known galaxy density, such as Stephen's Quintet. While the high galaxy densities suggest a short crossing-time and a strong dynamical interaction, the existence of numerous compact groups, each having a significant spiral fraction has provoked controversy regarding the reality of the compact groups, their age,__ and their state of dynamical evolution. -
X-Ray Spectral Variability of Seyfert 2 Galaxies
Astronomy & Astrophysics manuscript no. Seyfert c ESO 2018 February 27, 2018 X-ray spectral variability of Seyfert 2 galaxies Hern´andez-Garc´ıa, L.1; Masegosa, J.1; Gonz´alez-Mart´ın, O.2; M´arquez, I.1 1 Instituto de Astrof´ısica de Andaluc´ıa, CSIC, Glorieta de la Astronom´ıa, s/n, 18008 Granada, Spain e-mail: [email protected] 2 Centro de radioastronom´ıa y Astrof´ısica (CRyA-UNAM), 3-72 (Xangari), 8701, Morelia, Mexico Received XXXX; accepted YYYY ABSTRACT Context. Variability across the electromagnetic spectrum is a property of active galactic nuclei (AGN) that can help constrain the physical properties of these galaxies. Nonetheless, the way in which the changes happen and whether they occur in the same way in every AGN are still open questions. Aims. This is the third in a series of papers with the aim of studying the X-ray variability of different families of AGN. The main purpose of this work is to investigate the variability pattern(s) in a sample of optically selected Seyfert 2 galaxies. Methods. We use the 26 Seyfert 2s in the V´eron-Cetty and V´eron catalog with data available from Chandra and/or XMM–Newton public archives at different epochs, with timescales ranging from a few hours to years. All the spectra of the same source were simultaneously fitted, and we let different parameters vary in the model. Whenever possible, short-term variations from the analysis of the light curves and/or long-term UV flux variations were studied. We divided the sample into Compton-thick and Compton-thin candidates to account for the degree of obscuration. -
GHASP: an Halpha Kinematic Survey of Spiral and Irregular Galaxies - IV
GHASP: an Halpha kinematic survey of spiral and irregular galaxies - IV. 44 new velocity fields. Extension, shape and asymmetry of Halpha rotation curves P. Amram, C. Balkowski, J. Boulesteix, J.L. Gach, O. Garrido, M. Marcelin To cite this version: P. Amram, C. Balkowski, J. Boulesteix, J.L. Gach, O. Garrido, et al.. GHASP: an Halpha kinematic survey of spiral and irregular galaxies - IV. 44 new velocity fields. Extension, shape and asymmetry of Halpha rotation curves. Monthly Notices of the Royal Astronomical Society, Oxford University Press (OUP): Policy P - Oxford Open Option A, 2005, 362, pp.127. 10.1111/j.1365-2966.2005.09274.x. hal-00017198 HAL Id: hal-00017198 https://hal.archives-ouvertes.fr/hal-00017198 Submitted on 13 Dec 2020 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. Mon. Not. R. Astron. Soc. 362, 127–166 (2005) doi:10.1111/j.1365-2966.2005.09274.x GHASP: an Hα kinematic survey of spiral and irregular galaxies – IV. 44 new velocity fields. Extension, shape and asymmetry of Hα rotation curves , O. Garrido,1 2 M. Marcelin,2 P. Amram,2 C. Balkowski,1 J. -
Astronomy Magazine 2011 Index Subject Index
Astronomy Magazine 2011 Index Subject Index A AAVSO (American Association of Variable Star Observers), 6:18, 44–47, 7:58, 10:11 Abell 35 (Sharpless 2-313) (planetary nebula), 10:70 Abell 85 (supernova remnant), 8:70 Abell 1656 (Coma galaxy cluster), 11:56 Abell 1689 (galaxy cluster), 3:23 Abell 2218 (galaxy cluster), 11:68 Abell 2744 (Pandora's Cluster) (galaxy cluster), 10:20 Abell catalog planetary nebulae, 6:50–53 Acheron Fossae (feature on Mars), 11:36 Adirondack Astronomy Retreat, 5:16 Adobe Photoshop software, 6:64 AKATSUKI orbiter, 4:19 AL (Astronomical League), 7:17, 8:50–51 albedo, 8:12 Alexhelios (moon of 216 Kleopatra), 6:18 Altair (star), 9:15 amateur astronomy change in construction of portable telescopes, 1:70–73 discovery of asteroids, 12:56–60 ten tips for, 1:68–69 American Association of Variable Star Observers (AAVSO), 6:18, 44–47, 7:58, 10:11 American Astronomical Society decadal survey recommendations, 7:16 Lancelot M. Berkeley-New York Community Trust Prize for Meritorious Work in Astronomy, 3:19 Andromeda Galaxy (M31) image of, 11:26 stellar disks, 6:19 Antarctica, astronomical research in, 10:44–48 Antennae galaxies (NGC 4038 and NGC 4039), 11:32, 56 antimatter, 8:24–29 Antu Telescope, 11:37 APM 08279+5255 (quasar), 11:18 arcminutes, 10:51 arcseconds, 10:51 Arp 147 (galaxy pair), 6:19 Arp 188 (Tadpole Galaxy), 11:30 Arp 273 (galaxy pair), 11:65 Arp 299 (NGC 3690) (galaxy pair), 10:55–57 ARTEMIS spacecraft, 11:17 asteroid belt, origin of, 8:55 asteroids See also names of specific asteroids amateur discovery of, 12:62–63 -
Soft X-Ray Properties of a Spectroscopically Selected Sample of Interacting and Isolated Seyfert Galaxies?
A&A 368, 797–816 (2001) Astronomy DOI: 10.1051/0004-6361:20010055 & c ESO 2001 Astrophysics Soft X-ray properties of a spectroscopically selected sample of interacting and isolated Seyfert galaxies? F. Pfefferkorn1, Th. Boller1, and P. Rafanelli2 1 Max-Planck-Institut f¨ur extraterrestrische Physik, Postfach 1312, 85741 Garching, Germany 2 Department of Astronomy, University of Padova, Vicolo Osservatorio 5, 35122 Padova, Italy Received 12 October 2000 / Accepted 4 January 2001 Abstract. We present a catalogue of ROSAT detected sources in the sample of spectroscopically selected Seyfert 1 and Seyfert 2 galaxies of Rafanelli et al. (1995). The catalogue contains 102 Seyfert 1 and 36 Seyfert 2 galaxies. The identification is based on X-ray contour maps overlaid on optical images taken from the Digitized Sky Survey. We have derived the basic spectral and timing properties of the X-ray detected Seyfert galaxies. For Seyfert 1 galaxies a strong correlation between photon index and X-ray luminosity is detected. We confirm the presence of generally steeper X-ray continua in narrow-line Seyfert 1 galaxies (NLS1s) compared to broad-line Seyfert 1 galaxies. Seyfert 2 galaxies show photon indices similar to those of NLS1s. Whereas a tendency for an increasing X-ray luminosity with increasing interaction strength is found for Seyfert 1 galaxies, such a correlation is not found for Seyfert 2 galaxies. For Seyfert 1 galaxies we found also a strong correlation for increasing far-infrared luminosity with increasing interaction strength. Both NLS1s and Seyfert 2 galaxies show the highest values of far-infrared luminosity compared to Seyfert 1 galaxies, suggesting that NLS1s and Seyfert 2 galaxies host strong (circumnuclear) star formation. -
190 Index of Names
Index of names Ancora Leonis 389 NGC 3664, Arp 005 Andriscus Centauri 879 IC 3290 Anemodes Ceti 85 NGC 0864 Name CMG Identification Angelica Canum Venaticorum 659 NGC 5377 Accola Leonis 367 NGC 3489 Angulatus Ursae Majoris 247 NGC 2654 Acer Leonis 411 NGC 3832 Angulosus Virginis 450 NGC 4123, Mrk 1466 Acritobrachius Camelopardalis 833 IC 0356, Arp 213 Angusticlavia Ceti 102 NGC 1032 Actenista Apodis 891 IC 4633 Anomalus Piscis 804 NGC 7603, Arp 092, Mrk 0530 Actuosus Arietis 95 NGC 0972 Ansatus Antliae 303 NGC 3084 Aculeatus Canum Venaticorum 460 NGC 4183 Antarctica Mensae 865 IC 2051 Aculeus Piscium 9 NGC 0100 Antenna Australis Corvi 437 NGC 4039, Caldwell 61, Antennae, Arp 244 Acutifolium Canum Venaticorum 650 NGC 5297 Antenna Borealis Corvi 436 NGC 4038, Caldwell 60, Antennae, Arp 244 Adelus Ursae Majoris 668 NGC 5473 Anthemodes Cassiopeiae 34 NGC 0278 Adversus Comae Berenices 484 NGC 4298 Anticampe Centauri 550 NGC 4622 Aeluropus Lyncis 231 NGC 2445, Arp 143 Antirrhopus Virginis 532 NGC 4550 Aeola Canum Venaticorum 469 NGC 4220 Anulifera Carinae 226 NGC 2381 Aequanimus Draconis 705 NGC 5905 Anulus Grahamianus Volantis 955 ESO 034-IG011, AM0644-741, Graham's Ring Aequilibrata Eridani 122 NGC 1172 Aphenges Virginis 654 NGC 5334, IC 4338 Affinis Canum Venaticorum 449 NGC 4111 Apostrophus Fornac 159 NGC 1406 Agiton Aquarii 812 NGC 7721 Aquilops Gruis 911 IC 5267 Aglaea Comae Berenices 489 NGC 4314 Araneosus Camelopardalis 223 NGC 2336 Agrius Virginis 975 MCG -01-30-033, Arp 248, Wild's Triplet Aratrum Leonis 323 NGC 3239, Arp 263 Ahenea -
Making a Sky Atlas
Appendix A Making a Sky Atlas Although a number of very advanced sky atlases are now available in print, none is likely to be ideal for any given task. Published atlases will probably have too few or too many guide stars, too few or too many deep-sky objects plotted in them, wrong- size charts, etc. I found that with MegaStar I could design and make, specifically for my survey, a “just right” personalized atlas. My atlas consists of 108 charts, each about twenty square degrees in size, with guide stars down to magnitude 8.9. I used only the northernmost 78 charts, since I observed the sky only down to –35°. On the charts I plotted only the objects I wanted to observe. In addition I made enlargements of small, overcrowded areas (“quad charts”) as well as separate large-scale charts for the Virgo Galaxy Cluster, the latter with guide stars down to magnitude 11.4. I put the charts in plastic sheet protectors in a three-ring binder, taking them out and plac- ing them on my telescope mount’s clipboard as needed. To find an object I would use the 35 mm finder (except in the Virgo Cluster, where I used the 60 mm as the finder) to point the ensemble of telescopes at the indicated spot among the guide stars. If the object was not seen in the 35 mm, as it usually was not, I would then look in the larger telescopes. If the object was not immediately visible even in the primary telescope – a not uncommon occur- rence due to inexact initial pointing – I would then scan around for it. -
Arp Catalogue.Xlsx
ATLAS OF PECULIAR GALAXIES CATALOGUE 1 ATLAS OF PECULIAR GALAXIES CATALOGUE Object Name Mag RA Dec Constellation ARP 1 NGC 2857 12.2 09:24:37 49:21:00 Ursa Major ARP 2 13.2 16:16:18 47:02:00 Hercules ARP 3 13.4 22:36:34 ‐02:54:00 Aquarius ARP 4 13.7 01:48:25 ‐12:22:00 Cetus ARP 5 NGC 3664 12.8 11:24:24 03:19:00 Leo ARP 6 NGC 2537 12.3 08:13:14 45:59:00 Lynx ARP 7 14.5 08:50:17 ‐16:34:00 Hydra ARP 8 NGC 0497 13 01:22:23 ‐00:52:00 Cetus ARP 9 NGC 2523 11.9 08:14:59 73:34:00 Camelopardalis ARP 10 13.8 02:18:26 05:39:00 Cetus ARP 11 14.4 01:09:23 14:20:00 Pisces ARP 12 NGC 2608 12.2 08:35:17 28:28:00 Cancer ARP 13 NGC 7448 11.6 23:00:02 15:59:00 Pegasus ARP 14 NGC 7314 10.9 22:35:45 ‐26:03:00 Pisces Austrinus ARP 15 NGC 7393 12.6 22:51:39 ‐05:33:00 Aquarius ARP 16 M66 8.9 11:20:14 12:59:00 Leo ARP 17 14.7 07:44:32 73:49:00 Camelopardalis ARP 17 07:44:38 73:48:00 Camelopardalis ARP 18 NGC 4088 10.5 12:05:35 50:32:00 Ursa Major ARP 19 NGC 0145 13.2 00:31:45 ‐05:09:00 Cetus ARP 20 14.4 04:19:53 02:05:00 Taurus ARP 21 14.7 11:04:58 30:01:00 Leo Minor ARP 22 14.9 11:59:29 ‐19:19:00 Corvus ARP 22 NGC 4027 11.2 11:59:30 ‐19:15:00 Corvus ARP 23 NGC 4618 10.8 12:41:32 41:09:00 Canes Venatici ARP 24 NGC 3445 12.6 10:54:36 56:59:00 Ursa Major ARP 24 12.8 10:54:45 56:57:00 Ursa Major ARP 25 NGC 2276 11.4 07:27:13 85:45:00 Cepheus ARP 26 M101 7.9 14:03:12 54:21:00 Ursa Major ARP 27 NGC 3631 10.4 11:21:02 53:10:00 Ursa Major ARP 28 NGC 7678 11.8 23:28:27 22:25:00 Pegasus ARP 29 NGC 6946 8.8 20:34:52 60:09:00 Cygnus ARP 30 NGC 6365 12.2 17:22:42 62:10:00 -
The Dynamical Status of Stephan's Quintet
The dynamical status of Stephan’s Quintet M. Moles1,2, J. W. Sulentic3, and I. M´arquez4,5 ABSTRACT Multiwavelength data for Stephan’s Quintet (SQ) are consistent with the following model for this compact galaxy group. (1) Discordant redshift NGC 7320 is an unrelated foreground galaxy. (2) In the past SQ was an accordant redshift quartet involving NGC 7317, 18A, 19 and 20C. NGC 7320C collided (probably not for the first time) with the group a few times 108 years ago and stripped the interstellar matter from NGC 7319. (3) In the present SQ is again an accordant quartet involving NGC 7317, 18A,B, and 19. NGC 7318B is now entering the group at high velocity for the first time, giving rise to a shock zone. If most compact groups are like SQ, then they are frequently visited by infalling neighbors that perturb the group and themselves. SQ represents strong evidence for secondary infall in a small group environment. Tidal stripping reduces the mass of the infalling galaxies, thereby increasing the timescale for their orbital decay. There is little evidence that these high velocity “intruders” are rapidly captured and/or merge with the system. Instead they are the mechanism that sustains compact groups against collapse. Efficient gas stripping may account for the low star formation rate observed in compact groups and infall of residual gas into galactic nuclei may also foster the onset of active galactic nucleus activity. arXiv:astro-ph/9707194v1 16 Jul 1997 1Instituto de Matem´aticas y F´ısica Fundamental, CSIC, C/ Serrano 123, 28006 Madrid, Spain 2Observatorio Astron´omico Nacional, Madrid, Spain 3Department of Physics and Astronomy, University of Alabama, Tuscaloosa, USA 35487 4Institut d’Astrophysique de Paris, 98bis bd. -
Popular Names of Deep Sky (Galaxies,Nebulae and Clusters) Viciana’S List
POPULAR NAMES OF DEEP SKY (GALAXIES,NEBULAE AND CLUSTERS) VICIANA’S LIST 2ª version August 2014 There isn’t any astronomical guide or star chart without a list of popular names of deep sky objects. Given the huge amount of celestial bodies labeled only with a number, the popular names given to them serve as a friendly anchor in a broad and complicated science such as Astronomy The origin of these names is varied. Some of them come from mythology (Pleiades); others from their discoverer; some describe their shape or singularities; (for instance, a rotten egg, because of its odor); and others belong to a constellation (Great Orion Nebula); etc. The real popular names of celestial bodies are those that for some special characteristic, have been inspired by the imagination of astronomers and amateurs. The most complete list is proposed by SEDS (Students for the Exploration and Development of Space). Other sources that have been used to produce this illustrated dictionary are AstroSurf, Wikipedia, Astronomy Picture of the Day, Skymap computer program, Cartes du ciel and a large bibliography of THE NAMES OF THE UNIVERSE. If you know other name of popular deep sky objects and you think it is important to include them in the popular names’ list, please send it to [email protected] with at least three references from different websites. If you have a good photo of some of the deep sky objects, please send it with standard technical specifications and an optional comment. It will be published in the names of the Universe blog. It could also be included in the ILLUSTRATED DICTIONARY OF POPULAR NAMES OF DEEP SKY. -
Mid and Far Infrared Properties of a Complete Sample of Local Agns
Draft Version May 24, 2012 A Preprint typeset using LTEX style emulateapj v. 11/26/04 MID AND FAR INFRARED PROPERTIES OF A COMPLETE SAMPLE OF LOCAL AGNS Kohei Ichikawa1, Yoshihiro Ueda1, Yuichi Terashima2, Shinki Oyabu3, Poshak Gandhi4, Keiko Matsuta5, and Takao Nakagawa4 1 Department of Astronomy, Graduate School of Science, Kyoto University, Kitashirakawa-Oiwake cho, Kyoto, 606-8502, Japan 2 Department of Physics, Faculty of Science, Ehime University, Matsuyama 790-8577, Japan 3 Graduate School of Science, Nagoya University, Furo-cho, Chikusa-ku, Nagoya, Aichi 464-8602 Japan 4 Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo-ku, Sagamihara, Kanagawa 252-5210, Japan 5 Department of Space and Astronautical Science, The Graduate University for Advanced Studies, 3-1-1Yoshinodai, Chuo-ku, Sagamihara, Kanagawa 252-5210, Japan Draft Version May 24, 2012 ABSTRACT We investigate the mid- (MIR) to far-infrared (FIR) properties of a nearly complete sample of local Active Galactic Nuclei (AGNs) detected in the Swift/BAT all sky hard X-ray (14–195 keV) survey, based on the cross correlation with the AKARI infrared survey catalogs complemented by those with IRAS and WISE. Out of 135 non-blazer AGNs in the Swift/BAT 9 month catalog, we obtain the MIR photometric data for 128 sources either in the 9, 12, 18, 22, and/or 25 µm band. We find good correlation between their hard X-ray and MIR luminosities over 3 orders of magnitude (42 < log λLλ(9, 18 µm) < 45), which is tighter than that with the FIR luminosities at 90 µm.