The Expanding Universe
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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. -
Ngc Catalogue Ngc Catalogue
NGC CATALOGUE NGC CATALOGUE 1 NGC CATALOGUE Object # Common Name Type Constellation Magnitude RA Dec NGC 1 - Galaxy Pegasus 12.9 00:07:16 27:42:32 NGC 2 - Galaxy Pegasus 14.2 00:07:17 27:40:43 NGC 3 - Galaxy Pisces 13.3 00:07:17 08:18:05 NGC 4 - Galaxy Pisces 15.8 00:07:24 08:22:26 NGC 5 - Galaxy Andromeda 13.3 00:07:49 35:21:46 NGC 6 NGC 20 Galaxy Andromeda 13.1 00:09:33 33:18:32 NGC 7 - Galaxy Sculptor 13.9 00:08:21 -29:54:59 NGC 8 - Double Star Pegasus - 00:08:45 23:50:19 NGC 9 - Galaxy Pegasus 13.5 00:08:54 23:49:04 NGC 10 - Galaxy Sculptor 12.5 00:08:34 -33:51:28 NGC 11 - Galaxy Andromeda 13.7 00:08:42 37:26:53 NGC 12 - Galaxy Pisces 13.1 00:08:45 04:36:44 NGC 13 - Galaxy Andromeda 13.2 00:08:48 33:25:59 NGC 14 - Galaxy Pegasus 12.1 00:08:46 15:48:57 NGC 15 - Galaxy Pegasus 13.8 00:09:02 21:37:30 NGC 16 - Galaxy Pegasus 12.0 00:09:04 27:43:48 NGC 17 NGC 34 Galaxy Cetus 14.4 00:11:07 -12:06:28 NGC 18 - Double Star Pegasus - 00:09:23 27:43:56 NGC 19 - Galaxy Andromeda 13.3 00:10:41 32:58:58 NGC 20 See NGC 6 Galaxy Andromeda 13.1 00:09:33 33:18:32 NGC 21 NGC 29 Galaxy Andromeda 12.7 00:10:47 33:21:07 NGC 22 - Galaxy Pegasus 13.6 00:09:48 27:49:58 NGC 23 - Galaxy Pegasus 12.0 00:09:53 25:55:26 NGC 24 - Galaxy Sculptor 11.6 00:09:56 -24:57:52 NGC 25 - Galaxy Phoenix 13.0 00:09:59 -57:01:13 NGC 26 - Galaxy Pegasus 12.9 00:10:26 25:49:56 NGC 27 - Galaxy Andromeda 13.5 00:10:33 28:59:49 NGC 28 - Galaxy Phoenix 13.8 00:10:25 -56:59:20 NGC 29 See NGC 21 Galaxy Andromeda 12.7 00:10:47 33:21:07 NGC 30 - Double Star Pegasus - 00:10:51 21:58:39 -
Arxiv:1207.4189V1 [Astro-Ph.CO] 17 Jul 2012 N a Osdrtrefnaetlpyia Parame- Physical Fundamental Mass Three Alternatively, Ters: Consider Color
The Astrophysical Journal Supplement Series, in press, 17 July 2012 A Preprint typeset using LTEX style emulateapj v. 5/2/11 ANGULAR MOMENTUM AND GALAXY FORMATION REVISITED Aaron J. Romanowsky1, S. Michael Fall2 1University of California Observatories, Santa Cruz, CA 95064, USA 2Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA The Astrophysical Journal Supplement Series, in press, 17 July 2012 ABSTRACT Motivated by a new wave of kinematical tracers in the outer regions of early-type galaxies (ellipticals and lenticulars), we re-examine the role of angular momentum in galaxies of all types. We present new methods for quantifying the specific angular momentum j, focusing mainly on the more challenging case of early-type galaxies, in order to derive firm empirical relations between stellar j⋆ and mass M⋆ (thus extending the work by Fall 1983). We carry out detailed analyses of eight galaxies with kinematical data extending as far out as ten effective radii, and find that data at two effective radii are generally sufficient to estimate total j⋆ reliably. Our results contravene suggestions that ellipticals could harbor large reservoirs of hidden j⋆ in their outer regions owing to angular momentum transport in major mergers. We then carry out a comprehensive analysis of extended kinematic data from the literature for a sample of 100 nearby bright galaxies of all types, placing them on a diagram of ∼ j⋆ versus M⋆. The ellipticals and spirals form two parallel j⋆–M⋆ tracks, with log-slopes of 0.6, which for the spirals is closely related to the Tully-Fisher relation, but for the ellipticals derives from∼ a remarkable conspiracy between masses, sizes, and rotation velocities. -
The Black Hole Mass Function Derived from Local Spiral Galaxies
PUBLISHED IN THE ASTROPHYSICAL JOURNAL, 789:124 (16PP),2014 JULY 10 Preprint typeset using LATEX style emulateapj v. 12/16/11 THE BLACK HOLE MASS FUNCTION DERIVED FROM LOCAL SPIRAL GALAXIES BENJAMIN L. DAVIS1 , JOEL C. BERRIER1,2,5,LUCAS JOHNS3,6 ,DOUGLAS W. SHIELDS1,2, MATTHEW T. HARTLEY2,DANIEL KENNEFICK1,2, JULIA KENNEFICK1,2, MARC S. SEIGAR1,4 , AND CLAUD H.S. LACY1,2 Published in The Astrophysical Journal, 789:124 (16pp), 2014 July 10 ABSTRACT We present our determination of the nuclear supermassive black hole mass (SMBH) function for spiral galax- ies in the local universe, established from a volume-limited sample consisting of a statistically complete col- lection of the brightest spiral galaxies in the southern (δ< 0◦) hemisphere. Our SMBH mass function agrees well at the high-mass end with previous values given in the literature. At the low-mass end, inconsistencies exist in previous works that still need to be resolved, but our work is more in line with expectations based on modeling of black hole evolution. This low-mass end of the spectrum is critical to our understanding of the mass function and evolution of black holes since the epoch of maximum quasar activity. A limiting luminos- ity (redshift-independent) distance, DL = 25.4 Mpc (z =0.00572) and a limiting absolute B-band magnitude, MB = −19.12 define the sample. These limits define a sample of 140 spiral galaxies, with 128 measurable pitch angles to establish the pitch angle distribution for this sample. This pitch angle distribution function may be useful in the study of the morphology of late-type galaxies. -
Study of the Relation Between the Spiral Arm Pitch Angle and the Kinetic Energy of Random Motions of the Host Spiral Galaxies, a I
Journal of the Arkansas Academy of Science Volume 68 Article 7 2014 Study of the Relation between the Spiral Arm Pitch Angle and the Kinetic Energy of Random Motions of the Host Spiral Galaxies, A I. Al-Baidhany University of Arkansas at Little Rock, [email protected] M. Seigar University of Arkansas at Little Rock P. Treuthardt University of Arkansas at Little Rock A. Sierra University of Arkansas at Little Rock B. Davis University of Arkansas, Fayetteville See next page for additional authors Follow this and additional works at: http://scholarworks.uark.edu/jaas Part of the Physical Processes Commons Recommended Citation Al-Baidhany, I.; Seigar, M.; Treuthardt, P.; Sierra, A.; Davis, B.; Kennefick, D.; Kennefick, J.; Lacy, C.; Toma, Z. A.; and Jabbar, W. (2014) "Study of the Relation between the Spiral Arm Pitch Angle and the Kinetic Energy of Random Motions of the Host Spiral Galaxies, A," Journal of the Arkansas Academy of Science: Vol. 68 , Article 7. Available at: http://scholarworks.uark.edu/jaas/vol68/iss1/7 This article is available for use under the Creative Commons license: Attribution-NoDerivatives 4.0 International (CC BY-ND 4.0). Users are able to read, download, copy, print, distribute, search, link to the full texts of these articles, or use them for any other lawful purpose, without asking prior permission from the publisher or the author. This Article is brought to you for free and open access by ScholarWorks@UARK. It has been accepted for inclusion in Journal of the Arkansas Academy of Science by an authorized editor of ScholarWorks@UARK. -
A Classical Morphological Analysis of Galaxies in the Spitzer Survey Of
Accepted for publication in the Astrophysical Journal Supplement Series A Preprint typeset using LTEX style emulateapj v. 03/07/07 A CLASSICAL MORPHOLOGICAL ANALYSIS OF GALAXIES IN THE SPITZER SURVEY OF STELLAR STRUCTURE IN GALAXIES (S4G) Ronald J. Buta1, Kartik Sheth2, E. Athanassoula3, A. Bosma3, Johan H. Knapen4,5, Eija Laurikainen6,7, Heikki Salo6, Debra Elmegreen8, Luis C. Ho9,10,11, Dennis Zaritsky12, Helene Courtois13,14, Joannah L. Hinz12, Juan-Carlos Munoz-Mateos˜ 2,15, Taehyun Kim2,15,16, Michael W. Regan17, Dimitri A. Gadotti15, Armando Gil de Paz18, Jarkko Laine6, Kar´ın Menendez-Delmestre´ 19, Sebastien´ Comeron´ 6,7, Santiago Erroz Ferrer4,5, Mark Seibert20, Trisha Mizusawa2,21, Benne Holwerda22, Barry F. Madore20 Accepted for publication in the Astrophysical Journal Supplement Series ABSTRACT The Spitzer Survey of Stellar Structure in Galaxies (S4G) is the largest available database of deep, homogeneous middle-infrared (mid-IR) images of galaxies of all types. The survey, which includes 2352 nearby galaxies, reveals galaxy morphology only minimally affected by interstellar extinction. This paper presents an atlas and classifications of S4G galaxies in the Comprehensive de Vaucouleurs revised Hubble-Sandage (CVRHS) system. The CVRHS system follows the precepts of classical de Vaucouleurs (1959) morphology, modified to include recognition of other features such as inner, outer, and nuclear lenses, nuclear rings, bars, and disks, spheroidal galaxies, X patterns and box/peanut structures, OLR subclass outer rings and pseudorings, bar ansae and barlenses, parallel sequence late-types, thick disks, and embedded disks in 3D early-type systems. We show that our CVRHS classifications are internally consistent, and that nearly half of the S4G sample consists of extreme late-type systems (mostly bulgeless, pure disk galaxies) in the range Scd-Im. -
ASEM Newsletter December2015
ASEM Newsletter December2015 Comet C/2013 US10 Catalina December 1st, 2015 image from Gregg Ruppel December Calendar Social December 3 – 7-9pm Beginner Meeting @ Weldon Springs Interpretive Center, 7295 HWY 94 South, St. Charles, MO 63304 December 12 – Monthly Meeting. 5pm Open House, hors d’oeuvres @ Weldon Springs Interpretive Center, 7295 HWY 94 South, St. Charles, MO 63304. 6pm ham dinner provided by Marv and Barb Stewart followed by monthly meeting at 7pm. Complimentary dishes and desserts are welcome. Carla Kamp is turning over hospitality hosting duties with the January meeting. December 22- 7pm DigitalSIG Astrophoto group meeting Weldon Spring, 7295 Highway 94 South, St. Charles, MO 63304. Note this is the FOURTH Tuesday for just this month. We’ll go back to the 3rd Tuesday in January. December 23- 7PM DIY-ATMSIG Weldon Spring, 7295 Highway 94 South, St. Charles, MO 63304 December 4, 11, 18, 25- 7 pm start times Broemmelsiek Park Public viewing, weather permitting. ASTRONOMICAL DELIGHTS If you’re very careful, on December 7 a very old crescent moon will occult Venus in daylight, late morning. You’ll need to look to the west of the sun-don’t catch the sun in your binoculars- around 11:10 or so for the disappearance on the bright side of the moon. Start your search before 11am so you know where Venus and the moon are. Venus will be occulted for about 90 minutes. There’s a really good lunar libration on December 21 at the north Polar region. Good night to poke around the north polar landscape craters that are not normally discernible. -
Optical Follow-Up of Gravitational-Wave Events During the Second Advanced LIGO/ VIRGO Observing Run with the DLT40 Survey
The Astrophysical Journal, 875:59 (25pp), 2019 April 10 https://doi.org/10.3847/1538-4357/ab0e06 © 2019. The American Astronomical Society. All rights reserved. Optical Follow-up of Gravitational-wave Events during the Second Advanced LIGO/ VIRGO Observing Run with the DLT40 Survey Sheng Yang1,2,3 , David J. Sand4 , Stefano Valenti1 , Enrico Cappellaro3 , Leonardo Tartaglia4,5 , Samuel Wyatt4, Alessandra Corsi6 , Daniel E. Reichart7 , Joshua Haislip7, and Vladimir Kouprianov7,8 (DLT40 collaboration) 1 Department of Physics, University of California, 1 Shields Avenue, Davis, CA 95616-5270, USA; [email protected] 2 Department of Physics and Astronomy Galileo Galilei, University of Padova, Vicolo dell’Osservatorio, 3, I-35122 Padova, Italy 3 INAF Osservatorio Astronomico di Padova, Vicolo dell Osservatorio 5, I-35122 Padova, Italy 4 Department of Astronomy/Steward Observatory, 933 North Cherry Avenue, Room N204, Tucson, AZ 85721-0065, USA 5 Department of Astronomy and The Oskar Klein Centre, AlbaNova University Center, Stockholm University, SE-106 91 Stockholm, Sweden 6 Physics & Astronomy Department,Texas Tech University, Lubbock, TX 79409, USA 7 Department of Physics and Astronomy, University of North Carolina at Chapel Hill, Chapel Hill, NC 27599, USA 8 Central (Pulkovo) Observatory of Russian Academy of Sciences, 196140 Pulkovskoye Avenue 65/1, Saint Petersburg, Russia Received 2019 January 23; revised 2019 March 5; accepted 2019 March 6; published 2019 April 16 Abstract We describe the gravitational-wave (GW) follow-up strategy and subsequent results of the Distance Less Than 40 Mpc survey (DLT40) during the second science run (O2) of the Laser Interferometer Gravitational-wave Observatory and Virgo collaboration (LVC). -
Galaxies Hubble’S Tuning Fork Diagram E
Galaxies Hubble’s Tuning Fork Diagram E. Hubble (Tuning fork diagram) Different types of galaxies Structure, Size , populations Distance measurements Bizarre objects – Quasars- starlike object is 3C 273, Quasar Spiral Elliptical Irregular Spiral Galaxies Mass (M sun) 109 –1011 105 –1013 108 –1010 Luminosity 108 –1010 105 –1011 107 –109 ( L sun) M81: Sb galaxy Stellar I in disk Mostly II Mostly I NGC 1357: Sa galaxy NGC 4321: Sc galaxy populations II in halo and some I I – metal rich bulge II -metal poor Percentage of 77% 20% 3% observed galaxies NGC 4631: Sc galaxy NGC 891: Sb galaxy M104: Sa galaxy Andromeda (M32) Elliptical Galaxies Barred spiral galaxy M33: A Spiral Galaxy with Flocculent Spiral Arms M105: E0 galaxy M49: E4 galaxy NGC 4526: E7 galaxy Left: Large Magellanic Cloud, Irr 1 NGC 1365: SBc galaxy galaxy Right:NGC 4485 (Irr 2) M58: SBa galaxy and NGC 4490 (Sc) galaxies M74: a Grand Design Spiral Galaxy 1 The Hubble Law Five Galaxies V = H * D and Their H=71km/s/Mpc= 20km/s/Mly Distance = 10 million lys Spectra V=20km/s/Mly* 10mly=200km/s Distance = 100 million lys V=20km/s/Mly* 100mly =2000km/s Distance = 1 billion lys V=20km/s/Mly* 1000mly =20, 000km/s the age of the universe: 19 9 Ho = 3.09x10 km/Mpc = 13.6 x 10 years 71km/s/Mpc 13.6 billion yrs old Techniques for Measuring Clusters of Galaxies in Our Cosmological Distances Neighborhood Structure in the Universe The Local Group 2-Micron All Sky Survey Antlia: Recently Discovered Member of the Local Group Foamy Structure of the Universe The empty spaces in the foam are analogous to the voids found throughout the universe. -
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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 x x NGC 3511 GALXY CRT 11 03.4 -23 05 11 6 m 2.1 m 76 SBc vF,vL,mE 98 x x NGC 3513 GALXY CRT 11 03.8 -23 15 11.5 2.9 m 2.4 m 75 SBb vF,vL,mE 98 IC 2627 GALXY CRT 11 09.9 -23 44 12 2.6 m 2.1 m SBbc eF,L,R,stell N 98 NGC 3573 GALXY CEN 11 11.3 -36 53 12.3 3.6 m 1 m 4 Sa eF,S,R,glbM,3 st 11 f 98 NGC 3571 GALXY CRT 11 11.5 -18 17 12.1 3 m 0.9 m 94 SBa pF,pL,iF,bM 98 B,pL,E,vsmbMN,2 B st x NGC 3585 GALXY HYA 11 13.3 -26 45 9.9 5.2 m 3.1 m 107 Elliptical 98 tri NGC 3606 GALXY HYA 11 16.3 -33 50 12.4 1.5 m 1.4 m Elliptical eF,S,R,gbM 98 x x x NGC 3621 GALXY HYA 11 18.3 -32 49 9.7 12.4 m 5.7 m 159 SBcd cB,vL,E 160,am 4 st 98 NGC 3673 GALXY HYA 11 25.2 -26 44 11.5 3.7 m 2.4 m 70 SBb F,vL,gvlbM,*7 s 6' 98 PK 283+25.1 PLNNB HYA 11 26.7 -34 22 12.1 188 s 174 s 98 x NGC 3693 GALXY CRT 11 28.2 -13 12 13 3.4 m 0.7 m 85 Sb cF,S,E,gbM 98 NGC 3706 GALXY CEN 11 29.7 -36 24 11.3 3.1 m 1.8 m 78 E-SO pB,cS,R,psmbM 98 NGC 3717 GALXY HYA 11 31.5 -30 19 11.2 6.2 m 1 m 33 Sb pB,S,mE,*13 att 98 «ÆÊ¿ÀÄÀww«¸ÂÀ ¼¼ÇwªÂÐw¦¹Á¼ºËw£ÀÊËw II - C ll r l 400 e e l G C k i 200 r he Dec.