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CO Multi-Line Imaging of Nearby Galaxies (COMING) IV. Overview Of
Publ. Astron. Soc. Japan (2018) 00(0), 1–33 1 doi: 10.1093/pasj/xxx000 CO Multi-line Imaging of Nearby Galaxies (COMING) IV. Overview of the Project Kazuo SORAI1, 2, 3, 4, 5, Nario KUNO4, 5, Kazuyuki MURAOKA6, Yusuke MIYAMOTO7, 8, Hiroyuki KANEKO7, Hiroyuki NAKANISHI9 , Naomasa NAKAI4, 5, 10, Kazuki YANAGITANI6 , Takahiro TANAKA4, Yuya SATO4, Dragan SALAK10, Michiko UMEI2 , Kana MOROKUMA-MATSUI7, 8, 11, 12, Naoko MATSUMOTO13, 14, Saeko UENO9, Hsi-An PAN15, Yuto NOMA10, Tsutomu, T. TAKEUCHI16 , Moe YODA16, Mayu KURODA6, Atsushi YASUDA4 , Yoshiyuki YAJIMA2 , Nagisa OI17, Shugo SHIBATA2, Masumichi SETA10, Yoshimasa WATANABE4, 5, 18, Shoichiro KITA4, Ryusei KOMATSUZAKI4 , Ayumi KAJIKAWA2, 3, Yu YASHIMA2, 3, Suchetha COORAY16 , Hiroyuki BAJI6 , Yoko SEGAWA2 , Takami TASHIRO2 , Miho TAKEDA6, Nozomi KISHIDA2 , Takuya HATAKEYAMA4 , Yuto TOMIYASU4 and Chey SAITA9 1Department of Physics, Faculty of Science, Hokkaido University, Kita 10 Nishi 8, Kita-ku, Sapporo 060-0810, Japan 2Department of Cosmosciences, Graduate School of Science, Hokkaido University, Kita 10 Nishi 8, Kita-ku, Sapporo 060-0810, Japan 3Department of Physics, School of Science, Hokkaido University, Kita 10 Nishi 8, Kita-ku, Sapporo 060-0810, Japan 4Division of Physics, Faculty of Pure and Applied Sciences, University of Tsukuba, 1-1-1 Tennodai, Tsukuba, Ibaraki 305-8571, Japan 5Tomonaga Center for the History of the Universe (TCHoU), University of Tsukuba, 1-1-1 Tennodai, Tsukuba, Ibaraki 305-8571, Japan 6Department of Physical Science, Osaka Prefecture University, Gakuen 1-1, -
HST/WFC3 OBSERVATIONS of an OFF-NUCLEAR SUPERBUBBLE in ARP 220 Kelly E
The Astrophysical Journal, 810:149 (11pp), 2015 September 10 doi:10.1088/0004-637X/810/2/149 © 2015. The American Astronomical Society. All rights reserved. HST/WFC3 OBSERVATIONS OF AN OFF-NUCLEAR SUPERBUBBLE IN ARP 220 Kelly E. Lockhart1, Lisa J. Kewley2, Jessica R. Lu1, Mark G. Allen3, David Rupke4, Daniela Calzetti5, Richard I. Davies6, Michael A. Dopita2, Hauke Engel6, Timothy M. Heckman7, Claus Leitherer8, and David B. Sanders1 1 Institute for Astronomy, 2680 Woodlawn Drive, Honolulu, HI 96822, USA 2 Research School of Astronomy and Astrophysics, Australian National University, Cotter Road, Weston Creek ACT 2611, Australia 3 Observatoire de Strasbourg, UMR 7550, Strasbourg, F-67000, France 4 Department of Physics, Rhodes College, Memphis, TN 38112, USA 5 Department of Astronomy, University of Massachusetts, Amherst, MA 01003, USA 6 Max-Planck-Institut für Extraterrestrische Physik, Postfach 1312, D-85741 Garching, Germany 7 Center for Astrophysical Sciences, Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218, USA 8 Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA Received 2015 March 7; accepted 2015 June 8; published 2015 September 9 ABSTRACT We present a high spatial resolution optical and infrared study of the circumnuclear region in Arp 220, a late-stage galaxy merger. Narrowband imaging using Hubble Space Telescope/WFC3 has resolved the previously observed peak in Hα+[N II] emission into a bubble-shaped feature. This feature measures 1″. 6 in diameter, or 600 pc, and is only 1″ northwest of the western nucleus. The bubble is aligned with the western nucleus and the large-scale outflow axis seen in X-rays. -
The NICMOS Snapshot Survey of Nearby Galaxies
View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by CERN Document Server The NICMOS snapshot survey of nearby galaxies T. B¨oker1, D. Calzetti, W. Sparks, D. Axon1, L. E. Bergeron, H. Bushouse, L. Colina1, D. Daou, D. Gilmore, S. Holfeltz, J. MacKenty, L. Mazzuca, B. Monroe, J. Najita, K. Noll, A. Nota1,C. Ritchie, A. Schultz, M. Sosey, A. Storrs, A. Suchkov (the STScI NICMOS group) Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, U.S.A. ABSTRACT We present “snapshot” observations with the NearInfrared Camera and MultiObject Spectrometer (NICMOS) on board the Hubble Space Telescope (HST) of 94 nearby galaxies from the Revised Shapley Ames Catalog. Images with 0.200 resolution were obtained in two filters, a broad-band continuum filter (F160W, roughly equivalent to the H-band) and a narrow band filter centered on the Pa α line (F187N or F190N, depending on the galaxy redshift) with the 5100 5100 field of view of the NICMOS camera 3. A first- order continuum subtraction is performed,× and the resulting line maps and integrated Pa α line fluxes are presented. A statistical analysis indicates that the average Pa α surface brightness in the central regions is highest in early-type (Sa-Sb) spirals. Subject headings: infrared:galaxies—infrared:ISM:lines and bands—galaxies:nuclei— galaxies:starburst—galaxies:statistics 1Affiliated with the Astrophysics Division, Space Science Department, European Space Agency 1 1. Introduction with the NIC3 F190N filter. The velocity range was chosen such that the Pa α line falls well inside the NICMOS is a second generation HST instrument, high transmission region of the respective filter, with installed during the HST servicing mission in Febru- only minor corrections ( 5%) needed to account for ary 1997. -
Science in the Urantia Papers
Science ¾ Scientific Validation of the UB z By Denver Pearson z By Phil Calabrese ¾ Seraphic Velocities ¾ Astronomy The Scientific Integrity of the Urantia Book by Denver Pearson As scientifically minded readers first peruse the Urantia Book, it soon occurs to them that many of its statements on the natural sciences conflict with currently held data and theories. In the minds of many this gives rise to doubts about the truthfulness of those statements. Wisdom would lead us to realize that nothing short of perfection is perfect, and anything touched by human hands has fingerprints. This should be our guiding thoughts as we contemplate the accuracy of the scientific content of the Urantia Papers. Several years ago, at the first scientific symposium, it was implied by one of the speakers that the revelation contains errors. This implication is alarming. More recently, at the second symposium held in Oklahoma, an interesting publication named "The Science Content of The Urantia Book" was made available (this document is obtainable from the Brotherhood of Man Library). In this publication is an article entitled "Time Bombs" in which the author suggests that the revelators planted certain inaccurate scientific statements in the book in order to prevent it from becoming a fetish. He states "...the revelators incorporated safeguards in the papers that would form The Urantia Book to diminish the tendency to regard it as an object of worship. What safeguards did they use? Suppose they decided to make sure that mortals reading it understood that some cosmological statements in the book would be found to be inaccurate". -
Extra-Nuclear Starbursts: Young Luminous Hinge Clumps In
Extra-Nuclear Starbursts: Young Luminous Hinge Clumps in Interacting Galaxies Beverly J. Smith1, Roberto Soria2, Curtis Struck3, Mark L. Giroux1, Douglas A. Swartz4, and Mihoko Yukita5 ABSTRACT Hinge clumps are luminous knots of star formation near the base of tidal features in some interacting galaxies. We use archival Hubble Space Telescope UV/optical/IR images and Chandra X-ray maps along with GALEX UV, Spitzer IR, and ground-based optical/near-IR images to investigate the star forming properties in a sample of 12 hinge clumps in five interacting galaxies. 1 The most extreme of these hinge clumps have star formation rates of 1 9 M yr− , comparable to or larger than the ‘overlap’ region of intense star formation between− the⊙ two disks of the colliding galaxy system the Antennae. In the HST images, we have found remarkably large and luminous sources at the centers of these hinge clumps. These objects are much larger and more luminous than typical ‘super-star clusters’ in interacting galaxies, and are sometimes embedded in a linear ridge of fainter star clusters, consistent with star formation along a narrow caustic. These central sources have diameters of 70 pc, compared to 3 pc in ‘ordinary’ super-star clusters. ∼ ∼ Their absolute I magnitudes range from MI 12.2 to 16.5, thus if they are individual star clusters they would lie near the top of the ‘super∼ − star cluster’− luminosity function of star clusters. These sources may not be individual star clusters, but instead may be tightly packed groups of clusters that are blended together in the HST images. -
Mid-Infrared Images of Stars and Dust in Irregular Galaxies
Mid-Infrared Images of Stars and Dust in Irregular Galaxies1 Deidre A. Hunter2, Bruce G. Elmegreen3, and Emily Martin2,4 ABSTRACT We present mid-infrared to optical properties of 22 representative irregular galaxies: 18 Im, 3 BCDs, and one Sm. The mid-IR is based on images from the Spitzer Space Telescope archives. The 3.6 and 4.5 µm bands and the UBVJHK images are used to examine disk morphology and the integrated and azimuthally averaged magnitudes and colors of stars. The non-stellar contribution to the 4.5 µm images is used to trace hot dust. The 5.8 and 8.0 µm images reveal emission from hot dust and PAHs, and both may contribute to these passbands, although we refer to the non-stellar emission as PAH emission. We compare the 8.0 µm images to Hα. Im galaxies have no hidden bars, and those with double- exponential optical light profiles have the same at mid-IR. Most galaxies have similar optical and mid-IR scale lengths. Four galaxies have super star clusters that are not visible at optical bands. Galaxies with higher area-normalized star formation rates have more dust and PAH emission relative to starlight. Hot dust and PAH emission is found mostly in high surface brightness H ii regions, implying that massive stars are the primary source of heating. Galaxies with intense, wide-spread star formation have more extended PAH emission. The ratio of PAH to Hα emission is not constant on small scales. PAHs are associated with shells and giant filaments, so they are not destroyed during shell formation. -
And Ecclesiastical Cosmology
GSJ: VOLUME 6, ISSUE 3, MARCH 2018 101 GSJ: Volume 6, Issue 3, March 2018, Online: ISSN 2320-9186 www.globalscientificjournal.com DEMOLITION HUBBLE'S LAW, BIG BANG THE BASIS OF "MODERN" AND ECCLESIASTICAL COSMOLOGY Author: Weitter Duckss (Slavko Sedic) Zadar Croatia Pусскй Croatian „If two objects are represented by ball bearings and space-time by the stretching of a rubber sheet, the Doppler effect is caused by the rolling of ball bearings over the rubber sheet in order to achieve a particular motion. A cosmological red shift occurs when ball bearings get stuck on the sheet, which is stretched.“ Wikipedia OK, let's check that on our local group of galaxies (the table from my article „Where did the blue spectral shift inside the universe come from?“) galaxies, local groups Redshift km/s Blueshift km/s Sextans B (4.44 ± 0.23 Mly) 300 ± 0 Sextans A 324 ± 2 NGC 3109 403 ± 1 Tucana Dwarf 130 ± ? Leo I 285 ± 2 NGC 6822 -57 ± 2 Andromeda Galaxy -301 ± 1 Leo II (about 690,000 ly) 79 ± 1 Phoenix Dwarf 60 ± 30 SagDIG -79 ± 1 Aquarius Dwarf -141 ± 2 Wolf–Lundmark–Melotte -122 ± 2 Pisces Dwarf -287 ± 0 Antlia Dwarf 362 ± 0 Leo A 0.000067 (z) Pegasus Dwarf Spheroidal -354 ± 3 IC 10 -348 ± 1 NGC 185 -202 ± 3 Canes Venatici I ~ 31 GSJ© 2018 www.globalscientificjournal.com GSJ: VOLUME 6, ISSUE 3, MARCH 2018 102 Andromeda III -351 ± 9 Andromeda II -188 ± 3 Triangulum Galaxy -179 ± 3 Messier 110 -241 ± 3 NGC 147 (2.53 ± 0.11 Mly) -193 ± 3 Small Magellanic Cloud 0.000527 Large Magellanic Cloud - - M32 -200 ± 6 NGC 205 -241 ± 3 IC 1613 -234 ± 1 Carina Dwarf 230 ± 60 Sextans Dwarf 224 ± 2 Ursa Minor Dwarf (200 ± 30 kly) -247 ± 1 Draco Dwarf -292 ± 21 Cassiopeia Dwarf -307 ± 2 Ursa Major II Dwarf - 116 Leo IV 130 Leo V ( 585 kly) 173 Leo T -60 Bootes II -120 Pegasus Dwarf -183 ± 0 Sculptor Dwarf 110 ± 1 Etc. -
As101 Galaxy V2
Reminder 1. “Runaway Universe” assignment, with an in-class essay next week 2. Final Exam on 05/09 - Mandatory Presence; no make up - Closed online searches - Open book and open notes 3. Misc? This presentation on galaxy deviates from the textbook materials It is built with the next week’s presentation in mind Hubble’s Classification of Galaxies (Tuning Fork) http://en.wikipedia.org/wiki/Galaxy_morphological_classification MWG is SBb - Hubble Classification is improved upon by de Vaucouleurs We will see some examples of each type Let’s begin with our galactic neighbors The Whirlpool Galaxy M51 (M51a) (And companion M51b) Grand-design galaxy Self-sustaining star forming regions along spiral arm M51b: Lencular? (SB0) Amorphous? Irregular? Our Big Neighbors: M33 and M31 (Barred Spirals) http://tehgeektive.com/2012/06/12/what-happens-when-two-galaxies-collide-video/ Our Big Neighbors: M33 and M31 (Barred Spirals) http://apod.nasa.gov/apod/ap121220.html Triangulum Galaxy (Pinwheel) (M33, NGC 598) http://apod.nasa.gov/apod/ap080124.html Andromeda Galaxy (M31, NGC224) M32, a small elliptical dwarf, is above M110, a spheroidal dwarf, is below http:// annesastronomynews.com/annes-picture-of-the-day- the-andromeda-galaxy/ Andromeda - M31 - Barred Spiral http://apod.nasa.gov/apod/ap130202.html/ http://apod.nasa.gov/apod/ap120518.html Herschel Space Observatory (better than Spitzer) GALEX Bar can be seen! Hot Blue stars (O and B stars) Warm dust à will have star formation (now quiescent) Shows some ring structure – collision with M32? All about Andromeda -
Radio Astronom1y G
£t,: ,/ NATIONAL RADIO ASTRONOMY OBSERVATORY QUARTERLY REPORT October 1 - December 31, 1989 RADIO ASTRONOM1Y G.. '8 tO- C~oe'' n,'evI! I E. Vi. t-Li 1 2 1990 TABLE OF CONTENTS A. TELESCOPE USAGE ... .... ...... ............ 1 B. 140-FOOT OBSERVING PROGRAMS . .... .......... ... 1 C. 12-METER TELESCOPE ....... ..... ., .... ........ 5 D. VERY LARGE ARRAY ....... 1...................8 E. SCIENTIFIC HIGHLIGHTS .... ........ 19 F. PUBLICATIONS ............. G. CENTRAL DEVELOPMENT LABORATORY ........ 20 H. GREEN BANK ELECTRONICS . .. .a.. ...... 21 I. 12-METER ELECTRONICS ...... .. 0. I. 22 J. VLA ELECTRONICS ...... 0..... ..... .... a. 24 K. AIPS .... .............. ...... ............. 26 L. VLA COMPUTER ............. .. .0. .0. ... 27 M. VERY LONG BASELINE ARRAY . .. .0 .0 .0 .0 .0 . .0 .. 27 N. PERSONNEL .. ...... .... .0.0 . .0. .0. .. e. 30 APPENDIX A: List of NRAO Preprints A. TELESCOPE USAGE The NRAO telescopes have been scheduled for research and maintenance in the following manner during the fourth quarter of 1989. 140-ft 12-m VLA Scheduled observing (hrs) 1901.75 1583.50 1565.2 Scheduled maintenance and equipment changes 132.00 107.75 259.8 Scheduled tests and calibrations 20.75 425.75 327.1 Time lost 139.25 208.25 107.0 Actual observing 1762.50 1375.25 1458.2 B. 140-FOOT OBSERVING PROGRAMS The following line programs were conducted during this quarter. No. Observer(s) Program A-95 Avery, L (Herzberg) Observations at 18.2, 18.6, and Bell, M. (Herzberg) 23.7 GHz of cyanopolyynes in carbon Feldman, P. (Herzberg) stars part II. MacLeod, J. (Herzberg) Matthews, H. (Herzberg) B-493 Bania, T. (Boston) Measurements at 8.666 GHz of 3He + Rood, R. (Virginia) emission in HII regions and planetary Wilson, T. -
Bibliography of Refereed Papers: Roger L
Bibliography of refereed papers: Roger L. Davies 203 refereed papers, >24,000 citations, h=75 62 papers >100 citations; 13 papers >500 citations and one has more than 1000 citations. [203] Francesco D'Eugenio, Matthew Colless, Nicholas Scott, Arjen van der Wel, Roger L. Davies, Jesse van de Sande, Sarah M. Sweet, Sree Oh, Brent Groves, Rob Sharp, Matt S. Owers, Joss Bland-Hawthorn, Scott M. Croom, Sarah Brough, Julia J. Bryant, Michael Goodwin, Jon S. Lawrence, Nuria P. F. Lorente, and Samuel N. Richards. The SAMI Galaxy Survey: stellar population and structural trends across the Fundamental Plane. MNRAS, April 2021. [202] Scott M. Croom, Matt S. Owers, Nicholas Scott, Henry Poetrodjojo, Brent Groves, Jesse van de Sande, Tania M. Barone, Luca Cortese, Francesco D'Eugenio, Joss Bland-Hawthorn, Julia Bryant, Sree Oh, Sarah Brough, James Agostino, Sarah Casura, Barbara Catinella, Matthew Colless, Gerald Cecil, Roger L. Davies, Michael J. Drinkwater, Simon P. Driver, Ignacio Ferreras, Caroline Foster, Amelia Fraser-McKelvie, Jon Lawrence, Sarah K. Leslie, Jochen Liske, Angel´ R. L´opez-S´anchez, Nuria P. F. Lorente, Rebecca McElroy, Anne M. Medling, Danail Obreschkow, Samuel N. Richards, Rob Sharp, Sarah M. Sweet, Dan S. Taranu, Edward N. Taylor, Edoardo Tescari, Adam D. Thomas, James Tocknell, and Sam P. Vaughan. The SAMI Galaxy Survey: the third and final data release. MNRAS, February 2021. [201] Romina Ahumada and others. The 16th Data Release of the Sloan Digital Sky Surveys: First Release from the APOGEE-2 Southern Survey and Full Release of eBOSS Spectra. ApJS, 249(1):3, July 2020. [200] S. -
Cetus - the Whale
May 18 2021 Cetus - The Whale Observed: No Object Her Type Mag Alias/Notes IC 5384 Non-Existent NGC 7813 MCG -2-1-16 MK 936 IRAS 15-1215 PGC 287 IC 1528 Non-Existent NGC 7826 H29-8 Non-Existent Asterism IC 1533 Non-Existent NGC 34 Non-Existent NGC 17 NGC 58 Non-Existent NGC 47 PGC 967 MCG -1-1-55 IRAS 119-726 NGC 54 Glxy SB(r)a? 14.6 MCG -1-1-60 PGC 1011 NGC 59 Glxy SA(rs)0-: 13.1 ESO 539-4 MCG -4-1-26 PGC 1034 NGC 62 Glxy (R)SB(r)a: 12.3 MCG -2-1-43 IRAS 145-1345 PGC 1125 NGC 64 Glxy SB(s)bc 14 MCG -1-1-68 IRAS 149-706 PGC 1149 IC 5 Glxy E 14.8 MCG -2-1-47 IRAS 148-951 PGC 1145 NGC 73 Glxy SAB(rs)bc: 13.5 MCG -3-1-26 PGC 1211 NGC 65 Glxy SAB(rs)0-: 14.4 ESO 473-10A MCG -4-2-1 PGC 1229 NGC 66 Glxy SB(r)b pec 14.2 ESO 473-10 MCG -4-2-2 IRAS 165-2312 PGC 1236 IC 9 Glxy Sb(r) 16.1 MCG -2-2-1 IRAS 171-1423 PGC 1271 NGC 77 Glxy SA0-: 15.7 ESO 473-15 PGC 1290 NGC 102 Glxy S0/a 14.4 MCG -2-2-11 PGC 1542 NGC 107 Glxy Sbc 14.6 MCG -2-2-14 PGC 1606 NGC 111 Non-Existent NGC 113 Glxy SA0-: 13.5 MCG -1-2-16 PGC 1656 NGC 114 Glxy SB(rs)0: 14.7 UGC 259 MCG 0-2-27 MK 946 CGCG 383-14 KUG 24-20A PGC 1660 NGC 116 Non-Existent MCG -1-2-17 PGC 1671 NGC 117 Glxy S0+: sp 15.3 MCG 0-2-29 CGCG 383-15 PGC 1674 NGC 118 Glxy I0? 14.8 UGC 264 MCG 0-2-32 MK 947 CGCG 383-16 UM244 3ZW9 IRAS 247-203 PGC 1678 NGC 120 Glxy SB0^: 14.4 UGC 267 MCG 0-2-33 CGCG 383-17 PGC 1693 NGC 122 Non-Existent NGC 123 Non-Existent NGC 124 Glxy SA(s)c 13.7 UGC 271 MCG 0-2-38 CGCG 383-18 IRAS 253-205 PGC 1715 IC 15 Non-Existent IC 16 Glxy E? 14.7 MCG -2-2-17 IRAS 255-1322 PGC 1730 IC 17 -
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¼¼ÇwªÂÐw¦¹Á¼ºËw£ÀÊËw II - C ll r l 400 e e l G C k i 200 r he Dec. P.A. w R.A. Size Size Chart N a he ss d l Object Type Con. Mag. Class t NGC Description l AS o o sc e s r ( h m ) max min No. C a ( ' ) ( ) sc R AAS e r e M C T e B H H NGC 7192 GALXY IND 22 06.8 -64 19 11.2 1.9 m 1.8 m Elliptical pB,S,R,pmbM 134 NGC 7219 GALXY TUC 22 13.1 -64 51 12.5 1.7 m 1 m 27 SBa pB,S,R,2st nr 134 NGC 7329 GALXY TUC 22 40.4 -66 29 11.3 3.7 m 2.7 m 107 SBbc Ring pB,pS,mE90 134 NGC 7417 GALXY TUC 22 57.8 -65 02 12.3 1.9 m 1.3 m 2 SBab Ring pB,cS,R,gpmbM 134 NGC 7637 GALXY OCT 23 26.5 -81 55 12.5 2.1 m 1.9 m Sc vF,pL,R,vlbM,* nr 134 «ÆÊ¿ÀÄÀww«¸ÂÀ ¼¼ÇwªÂÐw¦¹Á¼ºËw£ÀÊËw II - C ll r l 400 e e l G C k i 200 r he Dec. P.A. w R.A. Size Size Chart N a he ss d l Object Type Con. Mag. Class t NGC Description l AS o o sc e s r ( h m ) max min No. C a ( ' ) ( ) sc R AAS e r e M C T e B H H Mel 227 OPNCL OCT 20 12.1 -79 19 5.3 50.0 m II 2 p 135 NGC 6872 GALXY PAV 20 17.0 -70 46 11.8 6.3 m 2.2 m 66 SBb/P F,pS,lE,glbM,1st of 4 135 NGC 6876 GALXY PAV 20 18.3 -70 52 11.1 3 m 2.6 m 80 E3 pB,S,R,eS* sf,2nd of 4 135 NGC 6877 GALXY PAV 20 18.6 -70 51 12.2 2 m 1 m 169 E6 vF,vS,R,3rd of 4 135 NGC 6880 GALXY PAV 20 19.5 -70 52 12.2 2.1 m 1.3 m 35 SBO-a F,S,R,r,vS* att,4 of 4 135 NGC 6920 GALXY OCT 20 44.0 -80 00 12.5 1.8 m 1.5 m SO pB,cS,R,psmbM 135 NGC 6943 GALXY PAV 20 44.6 -68 45 11.4 4 m 2.2 m 130 SBc pF,L,mE,vglbM vS* 135 IC 5052 GALXY PAV 20 52.1 -69 12 11.2 5.9 m 0.9 m 143 SBcd F,L,eE 140 deg 135 NGC 7020 GALXY PAV 21 11.3 -64 02 11.8 3.5 m 1.6 m 165 SBO-a Ring pB,cS,lE,pgbM 135 NGC 7083 GALXY IND 21 35.7 -63 54 11.2 3.6 m 2.1 m 5 Sbc pF,cL,vlE,vgpmbM,r 135 NGC 7096 GALXY IND 21 41.3 -63 55 11.9 1.8 m 1.6 m 130 Sa vF,S,R,vS** nf 135 NGC 7098 GALXY OCT 21 44.3 -75 07 11.3 4 m 2.6 m 74 SB Ring pF,R,g,psmbM,am st 135 NGC 7095 GALXY OCT 21 52.4 -81 32 11.5 4 m 3.3 m Sc F,pL,R,vglbM,*13 inv 135 «ÆÊ¿ÀÄÀww«¸ÂÀ ¼¼ÇwªÂÐw¦¹Á¼ºËw£ÀÊËw II - C ll r l 400 e e l G C k i 200 r he Dec.