Fundamental Astrophysics Course Lecture 1 - Overview
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38 Octans - Chamaleon SkyTools 3 / Skyhound.com β NGC 6025 NGC 2516 IC 2448 β β ε γ Chamaeleon Volans δ ε ε PK 315-13.1 Triangulum Australe β γ 12h δ2 α ε 3195 ζ PK 325-12.1 1 α ζ 6101 5h η θ δ α Apus 09h 2 IC 4499 γ δ1 β γ ζ 6362 η 2 2210 η 2164 18h 06h Large Magellanic Cloud Tarantula Nebulaδ Mensa 2031 NGC 2014 NGC 1962 NGC 1955 ζ NGC 1874 NGC 1829 θ 1866 κ NGC 1770 1805 Collinder 411 NGC 1814 1978 1818 1783 03h 6744 21h β ε ε γ Octans Pavo ν -80° 00h ν 1559 β α δ θ Hydrus Reticulum β γ ι δ 1313 β Small Magellanic Cloud 0° 52° x 34° -7 ε ζ κ 00h00m00.0s -90°00'00" (Skymark) Globular Cl. Dark Neb. Galaxy 8 7 6 5 4 3 2 1 Globule Planetary Open Cl. Nebula 38 Octans - Chamaleon GALASSIE Sigla Nome Cost. A.R. Dec. Mv. Dim. Tipo Distanza 200/4 80/11,5 20x60 NGC 292 Small Magellanic Cloud Tuc 00h 52m 38s +72° 48' 01” +2,80 318',0x204',0 SBm 0,2 Mly --- --- --- NGC 1313 Ret 03h 18m 15s -66° 29' 51” +9,70 9',5x7',2 Sbcd 13,5 Mly --- --- --- NGC 1559 Ret 04h 17m 36s -62° 47' 01" +11,00 4',2x2',1 SBc 34,0 Mly --- --- --- PGC 17223 Large Magellanic Cloud Dor 05h 23m 35s -69° 45' 22" +0,80 648',0x552',0 SBm 0,2 Mly --- --- --- NGC 6744 Pav 19h 09m 46s -63° 51' 28" +9,10 17',0x10',7 SABb 21,0 Mly --- --- --- AMMASSI APERTI Sigla Nome Cost. -
The Messenger
THE MESSENGER No, 40 - June 1985 Radial Veloeities of Stars in Globular Clusters: a Look into CD Cen and 47 Tue M. Mayor and G. Meylan, Geneva Observatory, Switzerland Subjected to dynamical investigations since the beginning photometry of several clusters reveals a cusp in the luminosity of the century, globular clusters still provide astrophysicists function of the central region, which could be the first evidence with theoretical and observational problems, wh ich so far have for collapsed cores. only been partly solved. The development of photoelectric cross-corelation tech If for a long time the star density projected on the sky was niques for the determination of stellar radial velocities opened fairly weil represented by simple dynamical models, recent the door to kinematical investigations (Gunn and Griffin, 1979, N .~- .", '. '.'., .' 1 '&307 w E ,. 1~ S Fig. 1: Left: 47 Tue (NGC 104) from the Deep Blue Survey - SRC-(J). Right: Centre of 47 Tue from a near-infrared photometrie study of Lioyd Evans. The diameter ofthe large eirele eorresponds to the disk ofthe left photograph. The maximum ofthe rotation appears inside the eircle; the linear part of the rotation eurve (solid-body rotation) affeets only stars inside one areminute of the eentre. 1 Rlre J 250r;.' .;r2' -i4.:...__.....;6;.;.. .;rB. ,;.;10::....--. Tentative Time-table of Council Sessions (J lkm/5] and Committee Meetings in 1985 (.) Gen x =2. November 12 Scientific Technical Committee November 13-14 Finance Committee December 11 -12 Observing Programmes Committee December 16 Committee of Council December 17 Council 10. All meetings will take place at ESO in Garching. -
407 a Abell Galaxy Cluster S 373 (AGC S 373) , 351–353 Achromat
Index A Barnard 72 , 210–211 Abell Galaxy Cluster S 373 (AGC S 373) , Barnard, E.E. , 5, 389 351–353 Barnard’s loop , 5–8 Achromat , 365 Barred-ring spiral galaxy , 235 Adaptive optics (AO) , 377, 378 Barred spiral galaxy , 146, 263, 295, 345, 354 AGC S 373. See Abell Galaxy Cluster Bean Nebulae , 303–305 S 373 (AGC S 373) Bernes 145 , 132, 138, 139 Alnitak , 11 Bernes 157 , 224–226 Alpha Centauri , 129, 151 Beta Centauri , 134, 156 Angular diameter , 364 Beta Chamaeleontis , 269, 275 Antares , 129, 169, 195, 230 Beta Crucis , 137 Anteater Nebula , 184, 222–226 Beta Orionis , 18 Antennae galaxies , 114–115 Bias frames , 393, 398 Antlia , 104, 108, 116 Binning , 391, 392, 398, 404 Apochromat , 365 Black Arrow Cluster , 73, 93, 94 Apus , 240, 248 Blue Straggler Cluster , 169, 170 Aquarius , 339, 342 Bok, B. , 151 Ara , 163, 169, 181, 230 Bok Globules , 98, 216, 269 Arcminutes (arcmins) , 288, 383, 384 Box Nebula , 132, 147, 149 Arcseconds (arcsecs) , 364, 370, 371, 397 Bug Nebula , 184, 190, 192 Arditti, D. , 382 Butterfl y Cluster , 184, 204–205 Arp 245 , 105–106 Bypass (VSNR) , 34, 38, 42–44 AstroArt , 396, 406 Autoguider , 370, 371, 376, 377, 388, 389, 396 Autoguiding , 370, 376–378, 380, 388, 389 C Caldwell Catalogue , 241 Calibration frames , 392–394, 396, B 398–399 B 257 , 198 Camera cool down , 386–387 Barnard 33 , 11–14 Campbell, C.T. , 151 Barnard 47 , 195–197 Canes Venatici , 357 Barnard 51 , 195–197 Canis Major , 4, 17, 21 S. Chadwick and I. Cooper, Imaging the Southern Sky: An Amateur Astronomer’s Guide, 407 Patrick Moore’s Practical -
Arxiv:1802.01597V1 [Astro-Ph.GA] 5 Feb 2018 Born 1991)
Astronomy & Astrophysics manuscript no. AA_2017_32084 c ESO 2018 February 7, 2018 Mapping the core of the Tarantula Nebula with VLT-MUSE? I. Spectral and nebular content around R136 N. Castro1, P. A. Crowther2, C. J. Evans3, J. Mackey4, N. Castro-Rodriguez5; 6; 7, J. S. Vink8, J. Melnick9 and F. Selman9 1 Department of Astronomy, University of Michigan, 1085 S. University Avenue, Ann Arbor, MI 48109-1107, USA e-mail: [email protected] 2 Department of Physics & Astronomy, University of Sheffield, Hounsfield Road, Sheffield, S3 7RH, UK 3 UK Astronomy Technology Centre, Royal Observatory, Blackford Hill, Edinburgh, EH9 3HJ, UK 4 Dublin Institute for Advanced Studies, 31 Fitzwilliam Place, Dublin, Ireland 5 GRANTECAN S. A., E-38712, Breña Baja, La Palma, Spain 6 Instituto de Astrofísica de Canarias, E-38205 La Laguna, Spain 7 Departamento de Astrofísica, Universidad de La Laguna, E-38205 La Laguna, Spain 8 Armagh Observatory and Planetarium, College Hill, Armagh BT61 9DG, Northern Ireland, UK 9 European Southern Observatory, Alonso de Cordova 3107, Santiago, Chile February 7, 2018 ABSTRACT We introduce VLT-MUSE observations of the central 20 × 20 (30 × 30 pc) of the Tarantula Nebula in the Large Magellanic Cloud. The observations provide an unprecedented spectroscopic census of the massive stars and ionised gas in the vicinity of R136, the young, dense star cluster located in NGC 2070, at the heart of the richest star-forming region in the Local Group. Spectrophotometry and radial-velocity estimates of the nebular gas (superimposed on the stellar spectra) are provided for 2255 point sources extracted from the MUSE datacubes, and we present estimates of stellar radial velocities for 270 early-type stars (finding an average systemic velocity of 271 ± 41 km s−1). -
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 -
Giant Stellar Arcs in the Large Magellanic Cloud: a Possible Link with Past Activity of the Milky Way Nucleus
Giant stellar arcs in the Large Magellanic Cloud: a possible link with past activity of the Milky Way nucleus Yuri N. Efremov* Sternberg Astronomical Institute of the Lomonosov Moscow State University, Moscow 119992, Russia Accepted 2012 November 1. Received 2012 November 1; in original form 2012 September 7 ABSTRACT The origin of the giant stellar arcs in the LMC remains a controversial issue, discussed since 1966. No other star/cluster arc is so perfect a segment of a circle; moreover, there is another similar arc near-by. Many hypotheses were advanced to explain these arcs, and all but one of these were disproved. It was proposed in 2004 that origin of these arcs was due to the bow shock from the jet, which is intermittently fired by the Milky Way nucleus – and during the last episode of its activity the jet was pointed to the LMC. Quite recently evidence for such a jet has really appeared. We suppose it was once energetic enough to trigger star formation in the LMC, and if the jet opening angle was about 2°, it could push out HI gas from the region of about 2 kpc in size, forming a cavity LMC4, - but also squeezed two dense clouds, which occurred in the same area, causing the formation of stars along their surfaces facing the core of the MW. In result, spherical segments of the stellar shells might arise, visible now as the arcs of Quadrant and Sextant, the apices of which point to the center of the MW. This orientation of both arcs can be the key to unlocking their origin. -
Spitzer Analysis of HII Region Complexes in the Magellanic
DRAFT VERSION AUGUST 16, 2018 Preprint typeset using LATEX style emulateapj v. 04/20/08 SPITZER ANALYSIS OF H II REGION COMPLEXES IN THE MAGELLANIC CLOUDS: DETERMINING A SUITABLE MONOCHROMATIC OBSCURED STAR FORMATION INDICATOR B. LAWTON1,K.D.GORDON1,B.BABLER2,M.BLOCK3,A.D.BOLATTO4,S.BRACKER2,L.R.CARLSON5,C.W.ENGELBRACHT3, J. L. HORA6,R.INDEBETOUW7,S.C.MADDEN8,M.MEADE2,M.MEIXNER1,K.MISSELT3,M.S.OEY9,J.M.OLIVEIRA10, T. ROBITAILLE6,M.SEWILO1,B.SHIAO1 U. P. VIJH11 , AND B. WHITNEY12 Draft version August 16, 2018 ABSTRACT H II regionsare the birth places of stars, and as such they providethe best measure of current star formation rates (SFRs) in galaxies. The close proximity of the Magellanic Clouds allows us to probe the nature of these star forming regions at small spatial scales. To study the H II regions, we compute the bolometric infrared flux, or total infrared (TIR), by integrating the flux from 8 to 500 µm. The TIR provides a measure of the obscured star formation because the UV photons from hot young stars are absorbed by dust and re-emitted across the mid-to-far-infrared(IR) spectrum. We aim to determine the monochromatic IR band that most accurately traces the TIR and produces an accurate obscured SFR over large spatial scales. We present the spatial analysis, via aperture/annulusphotometry, of 16 Large Magellanic Cloud (LMC) and 16 Small Magellanic Cloud (SMC) H II region complexes using the Spitzer Space Telescope’s IRAC (3.6, 4.5, 8 µm) and MIPS (24,70, 160 µm) bands. -
The Messenger
THE MESSENGER No, 40 - June 1985 Radial Veloeities of Stars in Globular Clusters: a Look into CD Cen and 47 Tue M. Mayor and G. Meylan, Geneva Observatory, Switzerland Subjected to dynamical investigations since the beginning photometry of several clusters reveals a cusp in the luminosity of the century, globular clusters still provide astrophysicists function of the central region, which could be the first evidence with theoretical and observational problems, wh ich so far have for collapsed cores. only been partly solved. The development of photoelectric cross-corelation tech If for a long time the star density projected on the sky was niques for the determination of stellar radial velocities opened fairly weil represented by simple dynamical models, recent the door to kinematical investigations (Gunn and Griffin, 1979, N .~- .", '. '.'., .' 1 '&307 w E ,. 1~ S Fig. 1: Left: 47 Tue (NGC 104) from the Deep Blue Survey - SRC-(J). Right: Centre of 47 Tue from a near-infrared photometrie study of Lioyd Evans. The diameter ofthe large eirele eorresponds to the disk ofthe left photograph. The maximum ofthe rotation appears inside the eircle; the linear part of the rotation eurve (solid-body rotation) affeets only stars inside one areminute of the eentre. 1 Rlre J 250r;.' .;r2' -i4.:...__.....;6;.;.. .;rB. ,;.;10::....--. Tentative Time-table of Council Sessions (J lkm/5] and Committee Meetings in 1985 (.) Gen x =2. November 12 Scientific Technical Committee November 13-14 Finance Committee December 11 -12 Observing Programmes Committee December 16 Committee of Council December 17 Council 10. All meetings will take place at ESO in Garching. -
Open Clusters PAGING
Open Clusters in Turn Left at Orion (5th edition) Page Name Constellation RA Dec Chapter 193 NGC 129 Cassiopeia 0 H 29.8 min. 60° 14' North 210 NGC 220 Tucana 0 H 40.5 min. −73° 24' South 210 NGC 222 Tucana 0 H 40.7 min. −73° 23' South 210 NGC 231 Tucana 0 H 41.1 min. −73° 21' South 192 NGC 225 Cassiopeia 0 H 43.4 min. 61° 47' North 210 NGC 265 Tucana 0 H 47.2 min. −73° 29' South 202 NGC 188 Cepheus 0 H 47.5 min. 85° 15' North 210 NGC 330 Tucana 0 H 56.3 min. −72° 28' South 210 NGC 371 Tucana 1 H 3.4 min. −72° 4' South 210 NGC 376 Tucana 1 H 3.9 min. −72° 49' South 210 NGC 395 Tucana 1 H 5.1 min. −72° 0' South 210 NGC 460 Tucana 1 H 14.6 min. −73° 17' South 210 NGC 458 Tucana 1 H 14.9 min. −71° 33' South 193 NGC 436 Cassiopeia 1 H 15.5 min. 58° 49' North 210 NGC 465 Tucana 1 H 15.7 min. −73° 19' South 193 NGC 457 Cassiopeia 1 H 19.0 min. 58° 20' North 194 M103 Cassiopeia 1 H 33.2 min. 60° 42' North 179 NGC 604, in M33 Triangulum 1 H 34.5 min. 30° 47' October–December 195 NGC 637 Cassiopeia 1 H 41.8 min. 64° 2' North 195 NGC 654 Cassiopeia 1 H 43.9 min. 61° 54' North 195 NGC 659 Cassiopeia 1 H 44.2 min. -
Skytools Chart
33 Dorado - Carina SkyTools 3 / Skyhound.com NGC 2546 ν α - ζ 40° σ α δ Puppis η2 Collinder 173 τ β 2 γ Canopus γ1 1433 NGC 2547 Horologium Pictor γ δ IC 2395 γ NGC 2670 χ α 1566 -5 0° ζ 1553 1549 ο NGC 2669 1672 IC 2391 δ ε α β 1261 Carina NGC 2516 ε Dorado ι α δ 2 γ η 1559 δ 1978 1866 1818 1783 NGC 1955 1805 Reticulum IC 2488 θ 2867 2164 κ ι NGC 1962 Large Magellanic Cloud β δ 2210 PK 278-06.1 Volans NGC 1874 NGC 1965 β NGC 1770 Tarantula Nebula NGC 1876 IC 2501 2031 β γ2 1313 ε -60° 2808 α NGC 3114 ζ Mensa ζ α υ PK 285-09.1 IC 2448 ε 1 β 0 -70° h 3211 h 0 02 8 52° x 34° 6h γ h 0 δ 06h00m00.0s -60°00'00" (Skymark) Globular Cl. Dark Neb. Galaxy 8 7 6 5 4 3 2 1 Globule Planetary Open Cl. Nebula 33 Dorado - Carina GALASSIE Sigla Nome Cost. A.R. Dec. Mv. Dim. Tipo Distanza 200/4 80/11,5 20x60 NGC 1313 Ret 03h 18m 15s -66° 29' 51" +9,70 9',5x7',2 SBcd 13,5 Mly --- --- --- NGC 1433 Hor 03h 42m 02s -47° 13' 19" +10,80 6',2x3',6 Sba 43,0 Mly --- --- --- NGC 1549 Dor 04h 15m 45s -55° 35' 32" +10,70 5',0x4',3 E 42,0 Mly --- --- --- NGC 1553 Dor 04h 16m 10s -55° 46' 51" +10,30 6',2x4',1 S0 28,0 Mly --- --- --- NGC 1559 Ret 04h 17m 36s -62° 47' 01" +11,00 4',2x2',1 SBc 34,0 Mly --- --- --- NGC 1566 Dor 04h 20m 04s +54° 56' 16" +10,30 8',1 4',8 34,0 Mly --- --- --- NGC 1672 Dor 04h 45m 43s -59° 14' 51" +10,30 6',6x5',4 Sb 270,0 Mly --- --- --- PGC 17223 Large Magellanic Cloud Dor 05h 23m 35s -69° 45' 22" +0,80 648',0x552',0 SBm 0,2 Mly --- --- --- AMMASSI APERTI Sigla Nome Cost. -
Arxiv:1604.03549V2 [Astro-Ph.HE] 18 Jul 2016 1 Introduction
The Observer's Guide to the Gamma-Ray Burst Supernova Connection − Zach Cano1, Shan-Qin Wang2;3, Zi-Gao Dai2;3 and Xue-Feng Wu4;5 1Centre for Astrophysics and Cosmology, Science Institute, University of Iceland, Dunhagi 5, 107 Reykjavik, Iceland. ([email protected]) 2School of Astronomy and Space Science, Nanjing University, Nanjing 210093, China. ([email protected]) 3Key Laboratory of Modern Astronomy and Astrophysics (Nanjing University), Ministry of Education, China. 4Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210008, China. ([email protected]) 5Joint Center for Particle, Nuclear Physics and Cosmology, Nanjing University-Purple Mountain Observa- tory, Nanjing 210008, China. Abstract. In this review article we present an up-to-date progress report of the connection between long-duration (and their various sub-classes) gamma-ray bursts (GRBs) and their accompanying supernovae (SNe). The analysis presented here is from the point of view of an observer, with much of the emphasis placed on how observations, and the modelling of observations, have constrained what we known about GRB-SNe. We discuss their photometric and spectroscopic properties, their role as cosmological probes, including their measured luminosity decline relationships, and − how they can be used to measure the Hubble constant. We present a statistical analysis of their bolometric properties, and use this to determine the properties of the \average" GRB-SN: which 52 52 has a kinetic energy of EK 2:5 10 erg (σE = 1:8 10 erg), an ejecta mass of Mej ≈ × K × ≈ 6 M (σMej = 4 M ), a nickel mass of MNi 0:4 M (σMNi = 0:2 M ), an ejecta velocity −1 ≈ −1 at peak light of v 20; 000 km s (σvph = 8; 000 km s ), a peak bolometric luminosity of 43 −1≈ 43 −1 Lp 1 10 erg s (σL = 0:4 10 erg s ), and it reaches peak bolometric light in tp 13 days ≈ × p × ≈ (σtp = 2:7 days). -
Stars, Galaxies, and Beyond, 2012
Stars, Galaxies, and Beyond Summary of notes and materials related to University of Washington astronomy courses: ASTR 322 The Contents of Our Galaxy (Winter 2012, Professor Paula Szkody=PXS) & ASTR 323 Extragalactic Astronomy And Cosmology (Spring 2012, Professor Željko Ivezić=ZXI). Summary by Michael C. McGoodwin=MCM. Content last updated 6/29/2012 Rotated image of the Whirlpool Galaxy M51 (NGC 5194)1 from Hubble Space Telescope HST, with Companion Galaxy NGC 5195 (upper left), located in constellation Canes Venatici, January 2005. Galaxy is at 9.6 Megaparsec (Mpc)= 31.3x106 ly, width 9.6 arcmin, area ~27 square kiloparsecs (kpc2) 1 NGC = New General Catalog, http://en.wikipedia.org/wiki/New_General_Catalogue 2 http://hubblesite.org/newscenter/archive/releases/2005/12/image/a/ Page 1 of 249 Astrophysics_ASTR322_323_MCM_2012.docx 29 Jun 2012 Table of Contents Introduction ..................................................................................................................................................................... 3 Useful Symbols, Abbreviations and Web Links .................................................................................................................. 4 Basic Physical Quantities for the Sun and the Earth ........................................................................................................ 6 Basic Astronomical Terms, Concepts, and Tools (Chapter 1) ............................................................................................. 9 Distance Measures ......................................................................................................................................................