DOCSLIB.ORG

Appendix: the Greek Alphabet

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Appendix: the Greek Alphabet Appendix: The Greek Alphabet The Greek alphabet is still used to designate the brighter stars of each constellation. This method of identification was developed by German astronomer Johan Bayer in 1603 when he published Uranometria , the first star atlas covering the entire sky. α Alpha η Eta ν Nu τ Tau β Beta θ Theta ξ Xi υ Upsilon γ Gamma ι Iota ο Omicron φ Phi δ Delta κ Kappa π Pi χ Chi ε Epsilon λ Lambda ρ Rho ψ Psi ζ Zeta μ Mu σ Sigma ω Omega © Springer International Publishing Switzerland 2015 293 D. A. Jenkins, First Light and Beyond, The Patrick Moore Practical Astronomy Series, DOI 10.1007/978-3-319-18851-5 References 1 1. DiCecco, A., Becucci, R., Bono, G., et al. (2010). On the absolute age of the Globular Cluster M92. Publ Astron Soc Pacifi c, 122 (895), 991–999. 2. Hendry, M. A., Smartt, S. J., Crockett, R. M., et al. (2006). SN 2004A: another Type II-P supernova with a red supergiant progenitor. Mon Not R Astron Soc, 369 (3), 1303–1320. 3. Fitzsimmons, A. (1993). CCD Stromgren UVBY photometry of the young clusters NGC 1893, NGC 457, Berkeley 94 and Bochum 1. Astron Astrophys Suppl Ser, 99 (1), 15–29. ISSN 0365–0138. 4. Quinn, S. N., White, R. J., Latham, D. W., et al. (2012). Two “b”s in the beehive: the discovery of the fi rst hot Jupiters in an open cluster. Astrophys J Lett, 756 (2), Article ID. L33, 5 pages. 5. Kiss, L., Szabo, M., Balog, Z., et al. (2008). AAOmega radial velocities rule out current membership of the planetary nebula NGC 2438 in the open cluster M46. Mon Not R Astron Soc, 391 (1), 399–404. 6. Crampton, D., Cowley, A., Schade, D., et al. (1985). The M31 globular cluster system. Astrophys J, 288 , 494–513. Part 1 (ISSN 0004–637X). 7. Van Dyk, S., Schuyler, D., Zheng, W., et al. (2013). The progenitor of supernova 2011dh has vanished. Astrophys J Lett, 772 (2), Article ID L32, 5 pages. 8. Sato, M., Hirota, T., Honma, M., et al. (2007). Absolute proper motions of water masers in NGC 281 measured with VERA, astrophysical masers and their environments. Proc IAU Symp, 242 , 170–171. 9. Mundell, C., James, P., Loiseau, N., et al. (2004). The unusual tidal dwarf candidate in the merger system NGC 3227/3226: star formation in a tidal shock? Astrophys J, 614 (2), 648–657. 1 This research has made use of NASA’s Astrophysics Data System. © Springer International Publishing Switzerland 2015 295 D. A. Jenkins, First Light and Beyond, The Patrick Moore Practical Astronomy Series, DOI 10.1007/978-3-319-18851-5 Index A Binoviewer , 59, 79 Amalthea , 63, 198 Blue stragglers , 110, 222 Apparent motion , 3, 15, 25, 27, 36, 38 Books (astronomy) , 233, 252–254, 262, 263, Asterism(s) , 20–21, 22, 69, 92, 98, 106, 270, 286 111, 113, 117, 133, 135, 203, 205, Butterfl y Nebula , 216, 218 227, 286 Astronomical League , 195, 203, 227, 237, 240, 274, 284–288 C Astronomy Celestial directions , 4, 5, 9, 12, 15, 24, 28, apps , 22 29, 39 software , 8, 11, 36, 94, 95, 144, 148, 277 Celestial sphere , 5, 7, 8, 13, 29, Astrophotography , 3, 25, 39, 77, 239–250, 37–39, 82 254, 263, 273, 290 Chandra , 231, 238, 274 Aurora borealis , 1, 54, 55 Cleaning (telescope) , 36 Auto-guider , 245 Cleaning optics , 35 Averted vision , 87, 96, 97, 106, 117, 119, 129, Collimation , 33–35, 39, 60, 71, 286 147, 150, 156, 173 Collinder 399 , 227 Constellations , 3, 8, 9, 11–15, 17–25, 32, 37–39, 53, 56, 66, 68–70, 75, 81, 82, B 86, 89, 90–95, 106, 111, 113, 116, Barnard, E.E. , 15, 63, 83, 197, 198, 212, 259 117–119, 122, 128, 132, 133, 135, 136, Bayer designations , 129 143, 149, 150, 153, 156, 163, 168, 177, Beehive Cluster (M44) , 51, 89, 90, 116, 136 178, 184, 188, 190–192, 194, 204, 206, Binoculars , 15, 17, 21, 22, 24, 25, 27, 29, 31, 207, 214, 216–218, 220, 224, 227, 229, 37, 54, 59, 64–66, 70, 71, 81, 91, 92, 235, 241, 253, 256, 259, 269, 270, 272, 96–98, 100, 106, 110, 111, 116, 117, 277, 293 119, 129, 133, 135, 136, 145, 147, Coordinates , 2, 7, 8, 36, 37, 70, 77, 135, 148, 149–152, 156, 163, 166, 168, 178, 185, 250, 260–262 194, 216, 218, 229, 277, 286, 287, 290 Curtis, Heber , 141 © Springer International Publishing Switzerland 2015 297 D. A. Jenkins, First Light and Beyond, The Patrick Moore Practical Astronomy Series, DOI 10.1007/978-3-319-18851-5 298 Index D H Dark adaptation , 74, 95–96, 106, 235 Heliosphere , 4, 5 Dark sky site , 50, 79, 203, 238, 248, 269, Helix Nebula , 129, 130, 191 280, 284 Herschel, Caroline , 222, 224, 264 Deep sky observing , 69, 70, 90, 147, 194, 257, Herschel, William , 46, 111, 118, 141, 177, 258, 273 178, 184, 185, 188, 197, 198, 222, 227, Delisle, Joseph , 46 252, 258 Dew prevention , 73–74 Hubble, Edwin , 142, 143, 239 Dew shield , 74, 78 Hubble Telescope , 17, 55, 57, 119, 148, Direction , 3–15, 17, 24, 28–31, 37–39, 57, 66, 231, 269 81, 91–93, 97, 135, 163, 173, 224, 245, 252, 254, 269 Distance , 3–9, 15–17, 26–28, 38, 39, 72, 92, I 97–100, 106, 111, 121, 122, 129, 148, IC 405 , 229, 230 150, 155, 163, 166, 177, 185, 204, 216, IC 410 , 229, 230 217, 224, 227, 234, 272 IC 1029 , 207, 211 Dreyer, J. , 1 IC 1590 , 216 DSLR camera , 241–245 IC 5146 , 132 International Dark-Sky Association (IDA) , 49, 57, 151, 199–202, 234, 237, E 274, 289 Eskimo Nebula (NGC 2392) , 89, 90, 136 Internet telescope rental , 249–250 Eyepieces , 27, 28, 39, 70–74, 79, 80, 91, 93, iTelescope , 248–250 94, 147 L F Laser collimator , 34, 74 Field of view , 4, 25–29, 31, 36, 37, 39, 65, Light pollution , 24, 39, 47–49, 56–58, 61, 63, 66, 71–74, 77, 81, 86, 91–94, 96, 98, 68, 75, 76, 95, 119, 147, 197–203, 232, 99, 106, 119, 128, 136, 144, 145, 149, 234, 237, 284, 287–289, 292 152, 168, 173, 176, 178, 181, 216, 224, Light year , 3, 4, 9, 15, 17, 89, 97–101, 103, 227, 244 106, 110, 111, 116, 117, 119, 121, 122, Filter(s) , 75–76 129, 132, 133, 141–143, 148–150, 152, broadband , 75 156, 163, 166, 168, 173, 177, 178, 181, H-beta , 76 184, 185, 194, 204–207, 212, 214, moon , 75 216–218, 220, 222, 224, 227, 281 narrowband , 76, 95, 250 O-III , 76, 128, 129, 134, 204, 218, 220, 229 M Finderscopes , 4, 33, 37–38, 60, 66–68, 74, 78, M1 , 203, 204 81, 86, 91, 93, 94, 98, 116, 117, 128, M2 , 99, 100, 103, 129 136, 145, 147, 152, 178, 194, 205 M3 , 117 FITS Liberator , 247 M4 , 117 Flamsteed numbers , 20, 69, 129 M5 , 117 Focal length , 26, 72, 91 M6 , 117 Focal ratio , 26, 71, 72 M7 , 117, 133 F ratio , 241 M8 , 133 M13 , 98–101, 106, 117, 144, 145, 204, 216 G M15 , 99, 100, 103, 129, 224 Galaxies , 25, 32, 47, 55, 69, 76, 77, 135, M20 , 60, 95, 134 141–196, 198, 202–204, 207, 211, 214, M21 , 134 215, 224, 227, 239, 240, 271, 272, 286 M23 , 135, 216, 219 Index 299 M27 , 122, 128 N M31 , 60, 66, 141, 142, 144, 148–152, Nebulae , 46, 47, 55, 63, 69, 71, 75, 77, 166, 295 89–142, 144, 145, 147, 149, 151, 168, M33 , 37, 144, 148–152, 166 194–196, 198, 203, 214, 220, 223, 229, M34 , 212 239, 243, 244, 261, 286 M36 , 117 New General Catalog , 1, 198 M37 , 117 New moon , 56, 81, 98 M38 , 111, 113, 116 NGC 366 , 227 M41 , 110, 111, 122 NGC 457 , 107, 110, 147 M42 , 60, 118, 119, 121, 220 NGC 659 , 224 M43 , 119 NGC 681 , 188, 191, 192 M44 , 51, 89, 90, 116 NGC 869 , 89, 110, 112, 205 M46 , 121–123 NGC 884 , 89, 110, 112, 205 M50 , 218, 220 NGC 1122 , 212, 213 M51 , 141, 142, 156, 159, 166 NGC 1893 , 117 M57 , 118, 136, 137 NGC 1907 , 116, 117 M65 , 168, 171 NGC 1931 , 117 M66 , 168, 171 NGC 1977 , 214 M68 , 206 NGC 1981 , 214 M76 , 128, 129 NGC 2316 , 218, 220 M78 , 220, 222, 223 NGC 2392 , 89, 90, 136 M81 , 152, 155–157, 166 NGC 2438 , 121–123 M82 , 152, 155, 156, 166 NGC 3226 , 227, 229 M83 , 150–153, 166 NGC 3227 , 227, 229 M92 , 98–101, 216 NGC 3242 , 206 M95 , 29, 173 NGC 3367 , 173, 174 M96 , 173 NGC 3377 , 173, 174 M97 , 166, 167 NGC 3384 , 173 M101 , 156, 161, 163, 166, 181 NGC 3389 , 173 M103 , 106, 107, 110, 224 NGC 3596 , 227 M104 , 60, 141, 143, 163, 164, 166, 191 NGC 3628 , 168, 171 M105 , 173 NGC 3666 , 227 M108 , 166–168 NGC 4038 , 214 M109 , 168, 169 NGC 4039 , 214 Magnifi cation (eyepiece) , 4, 26, 34, 39, 57, 58, NGC 4361 , 206, 209 65–66, 68, 71, 72, 79, 91, 98, 106, 117, NGC 5128 , 204, 206 135–137, 147, 151, 156, 177, 194, 205, NGC 5139 , 204, 205 206, 241 NGC 5195 , 141, 142, 156 Magnitude , 8, 13, 15–20, 22, 25, 57, 68–70, NGC 5426 , 177–179 91–95, 99–101, 106, 110, 111, 116, NGC 5427 , 177–179 117, 119, 122, 128, 129, 132, 133, NGC 5660 , 207, 211, 212 135–137, 143, 144, 147–152, 155, 156, NGC 5673 , 207, 211 163, 166, 168, 171, 173, 176–178, 181, NGC 5676 , 207–212 184, 185, 188, 191, 195, 202, 204–207, NGC 5907 , 178, 181 212, 214, 216, 218, 220, 224, 227, 234, NGC 5963 , 184 245, 261, 272 NGC 5965 , 184 McNeil’s Nebula , 222 NGC 5987 , 181, 183, 184 Messier, Charles , 45–47, 62, 111, 133, 141, NGC 6144 , 117 150, 168, 197, 198, 203, 206, 262, NGC 6207 , 99, 101, 144, 145 264, 273 NGC 6210 , 205, 208 Meteor showers , 52, 53, 61, 270, 271 NGC 6231 , 116, 117 Motion , 3–25, 27, 36, 38, 80, 81, 201, 244, NGC 6302 , 216, 218 245, 290 NGC 6440 , 216, 219 300 Index NGC 6445 , 216, 219 R NGC 6960 , 216, 218, 220 Red dot fi nder , 15, 38, 60, 91, 98, 116, 136, 286 NGC 6992 , 216 Ring Nebula , 118, 136, 137 NGC 7009 , 137, 138 Rosette Nebula , 220, 222 NGC 7293 , 129 NGC 7331 , 184–186 NGC 7332 , 224, 227, 228 S NGC 7339 , 224, 227, 228 Shapley, Harlow , 141 NGC 7457 , 224, 225 Sketching , 80, 83, 147, 257, 273 NGC 7625 , 224, 226 SN 2004A , 99 NGC 7662 , 122, 126 Software (astronomy) , 8, 9, 11, 23, 29, 36, 68, NGC 7789 , 222, 224 93–95, 117, 144, 148, 240, 241, NGC 7814 , 185, 188, 189 243–248, 277, 283 NOAO , 19, 90, 103, 111, 113, 133, 134, Spectroscopy , 18, 202, 235, 240, 250 138, 142, 155, 167, 169, 171, 201, 205, Spitzer
Load more

Recommended publications
  • III. the Young Open Cluster NGC 1893 in the HII Region W8
    MNRAS 443, 454–473 (2014) doi:10.1093/mnras/stu1170 Sejong Open Cluster Survey (SOS) – III. The young open cluster NGC 1893 in the H II region W8 Beomdu Lim,1,2‹† Hwankyung Sung,2‹ Jinyoung S. Kim,3 Michael S. Bessell4 and Byeong-Gon Park1 1Korea Astronomy and Space Science Institute, 776 Daedeokdae-ro, Yuseong-gu, Daejeon 305-348, Korea 2Department of Astronomy and Space Science, Sejong University, 209 Neungdong-Ro, Gwangjin-gu, Seoul 143-747, Korea 3Steward Observatory, University of Arizona, 933 N. Cherry Ave. Tucson, AZ 85721-0065, USA 4Research School of Astronomy and Astrophysics, Australian National University, MSO, Cotter Road, Weston, ACT 2611, Australia Downloaded from Accepted 2014 June 11. Received 2014 June 10; in original form 2014 March 31 ABSTRACT http://mnras.oxfordjournals.org/ We present a UBVI and Hα photometric study of the young open cluster NGC 1893 in the H II region W8 (IC 410 or Sh 2-236). A total of 65 early-type members are selected from photometric diagrams. A mean reddening of the stars is E(B − V)=0.563 ± 0.083 mag. The published photometric data in the near- and mid-infrared passbands are used to test the reddening law towards the cluster, and we confirm that the reddening law is normal (RV = 3.1). Zero-age main-sequence fitting gives a distance modulus of V0 − MV = 12.7 ± 0.2 mag, equivalent to 3.5 ± 0.3 kpc. From Hα photometry, 125 Hα emission stars and candidates are identified as pre-main-sequence (PMS). The lists of young stellar objects and X-ray sources published by previous studies allow us to select a large number of PMS members down to at The Australian National University on September 16, 2014 1M.
    [Show full text]
  • Winter Constellations
    Winter Constellations *Orion *Canis Major *Monoceros *Canis Minor *Gemini *Auriga *Taurus *Eradinus *Lepus *Monoceros *Cancer *Lynx *Ursa Major *Ursa Minor *Draco *Camelopardalis *Cassiopeia *Cepheus *Andromeda *Perseus *Lacerta *Pegasus *Triangulum *Aries *Pisces *Cetus *Leo (rising) *Hydra (rising) *Canes Venatici (rising) Orion--Myth: Orion, the great ​ ​ hunter. In one myth, Orion boasted he would kill all the wild animals on the earth. But, the earth goddess Gaia, who was the protector of all animals, produced a gigantic scorpion, whose body was so heavily encased that Orion was unable to pierce through the armour, and was himself stung to death. His companion Artemis was greatly saddened and arranged for Orion to be immortalised among the stars. Scorpius, the scorpion, was placed on the opposite side of the sky so that Orion would never be hurt by it again. To this day, Orion is never seen in the sky at the same time as Scorpius. DSO’s ● ***M42 “Orion Nebula” (Neb) with Trapezium A stellar ​ ​ ​ nursery where new stars are being born, perhaps a thousand stars. These are immense clouds of interstellar gas and dust collapse inward to form stars, mainly of ionized hydrogen which gives off the red glow so dominant, and also ionized greenish oxygen gas. The youngest stars may be less than 300,000 years old, even as young as 10,000 years old (compared to the Sun, 4.6 billion years old). 1300 ly. ​ ​ 1 ● *M43--(Neb) “De Marin’s Nebula” The star-forming ​ “comma-shaped” region connected to the Orion Nebula. ● *M78--(Neb) Hard to see. A star-forming region connected to the ​ Orion Nebula.
    [Show full text]
  • 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.
    [Show full text]
  • April Constellations of the Month
    April Constellations of the Month Leo Small Scope Objects: Name R.A. Decl. Details M65! A large, bright Sa/Sb spiral galaxy. 7.8 x 1.6 arc minutes, magnitude 10.2. Very 11hr 18.9m +13° 05’ (NGC 3623) high surface brighness showing good detail in medium sized ‘scopes. M66! Another bright Sb galaxy, only 21 arc minutes from M65. Slightly brighter at mag. 11hr 20.2m +12° 59’ (NGC 3627) 9.7, measuring 8.0 x 2.5 arc minutes. M95 An easy SBb barred spiral, 4 x 3 arc minutes in size. Magnitude 10.5, with 10hr 44.0m +11° 42’ a bright central core. The bar and outer ring of material will require larger (NGC 3351) aperature and dark skies. M96 Another bright Sb spiral, about 42 arc minutes east of M95, but larger and 10hr 46.8m +11° 49’ (NGC 3368) brighter. 6 x 4 arc minutes, magnitude 10.1. Located about 48 arc minutes NNE of M96. This small elliptical galaxy measures M105 only 2 x 2.1 arc minutes, but at mag. 10.3 has very high surface brightness. 10hr 47.8m +12° 35’ (NGC 3379) Look for NGC 3384! (110NGC) and NGC 3389 (mag 11.0 and 12.2) which form a small triangle with M105. NGC 3384! 10hr 48.3m +12° 38’ See comment for M105. The brightest galaxy in Leo, this Sb/Sc spiral galaxy shines at mag. 9.5. Look for NGC 2903!! 09hr 32.2m +21° 30’ a hazy patch 11 x 4.7 arc minutes in size 1.5° south of l Leonis.
    [Show full text]
  • SUPERMASSIVE BLACK HOLES and THEIR HOST SPHEROIDS III. the MBH − Nsph CORRELATION
    The Astrophysical Journal, 821:88 (8pp), 2016 April 20 doi:10.3847/0004-637X/821/2/88 © 2016. The American Astronomical Society. All rights reserved. SUPERMASSIVE BLACK HOLES AND THEIR HOST SPHEROIDS. III. THE MBH–nsph CORRELATION Giulia A. D. Savorgnan Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, Victoria 3122, Australia; [email protected] Received 2015 December 6; accepted 2016 March 6; published 2016 April 13 ABSTRACT The Sérsic R1 n model is the best approximation known to date for describing the light distribution of stellar spheroidal and disk components, with the Sérsic index n providing a direct measure of the central radial concentration of stars. The Sérsic index of a galaxy’s spheroidal component, nsph, has been shown to tightly correlate with the mass of the central supermassive black hole, MBH.TheMnBH– sph correlation is also expected from other two well known scaling relations involving the spheroid luminosity, Lsph:theLsph–n sph and the MLBH– sph. Obtaining an accurate estimate of the spheroid Sérsic index requires a careful modeling of a galaxy’s light distribution and some studies have failed to recover a statistically significant MnBH– sph correlation. With the aim of re-investigating the MnBH– sph and other black hole mass scaling relations, we performed a detailed (i.e., bulge, disks, bars, spiral arms, rings, halo, nucleus, etc.) decomposition of 66 galaxies, with directly measured black hole masses, that had been imaged at 3.6 μm with Spitzer.Inthispaper,the third of this series, we present an analysis of the Lsph–n sph and MnBH– sph diagrams.
    [Show full text]
  • 2012 年發表 53 篇 1. Chang,Chan-Kao , Lai,Shao-Yu
    2012 年發表 53 篇 1. Chang,Chan-Kao , Lai,Shao-Yu , Ko,Chung-Ming, et al. , Information on the Milky Way from the 2MASS All Sky Star Count: Bimodal Color Distributions ,The Astrophysical Journal, Volume 759, Issue 2, 94, 10 p..( 2012) 2. Chen,W.P. , Hu,S.C.-L. , Errmann,R., et al. , A Possible Detection of Occultation by a Proto-planetary Clump in GM Cephei ,The Astrophysical Journal, Volume 751, Issue 2, 118, 5 p..( 2012) 3. Hwang,Chorng-Yuan , Tsai,Mengchun, Star Formation in the Central Kiloparsec of Nearby Active Galaxies ,Journal of Physics: Conference Series, Volume 372, Issue 1, id. 0120..( 2012) 4. Ip, W.-H., ENA diagnostics of auroral activity at Mars ,Planetary and Space Science, v. 63, pp. 83, (2012) 5. J.M. Nester and C.-H. Wang, Can torsion be treated as just another tensor field? ,International Journal of Modern Physics: Conference Series, v. 7, pp. 158, (2012) 6. Lee, C.-H., Riffeser, A., Koppenhoefer, J., et al., PAndromeda?First Results from the High-cadence Monitoring of M31 with Pan-STARRS 1 ,The Astronomical Journal, Volume 143, Issue 4, article id. 89, 16 pp. (2012) 7. Lin, Z.-Y., Lara, L. M., Vincent, J. B., and Ip, W.-H., Physical studies of 81P/Wild 2 from the last two apparitions ,Astronomy and Astrophysics, v. 537, pp. A101, (2012) 8. Ngeow, C.-C., On the Application of Wesenheit Function in Deriving Distance to Galactic Cepheids ,The Astrophysical Journal, v. 747, pp. 50, (2012) 9. Ngeow, C.-C., Kanbur, S. M., Bellinger, E. P., et al., Period- luminosity relations for Cepheid variables: from mid-infrared to multi- phase, Astrophysics and Space Science, v.
    [Show full text]
  • National Observatories
    Sidney C Wolff NOAO/DIR NATIONAL OPTICAL ASTRONOMY OBSERVATORIES NATIONAL OPTICAL ASTRONOMY OBSERVATORIES Cerro Tololo Inter-American Observatory Kitt Peak National Observatory National Solar Observatory La Serena, Chile Tucson, Arizona 85726 Sunspot, New Mexico 88349 ANNUAL REPORT October 1996 - September 1997 October 30,1997 TABLE OF CONTENTS L INTRODUCTION IL AURA BOARD m. SCffiNTDJIC PROGRAM A. Cerro Tololo Inter-American Observatory (CTIO) 1. The Search for High Z Supernovae 2. Nearby Stars and Planets 2 B. Kitt Peak National Observatory (KPNO) 3 1. The History of Star Formation in Distant Galaxies 3 2. Oxygen Abundance and the Age of the Universe 4 3. The Age of Elliptical Galaxies - Is There Enough Time? 5 C. National Solar Observatory (NSO) 5 1. Results from GONG 5 2. High-Resolution Images of Solar Magnetic Fields 6 3. Active Optics Control Loop Closed at the Sac Peak Vacuum Tower Telescope 7 IV. DIVISION OPERATIONS 7 A. CTIO 7 Telescope Upgrades and Instrumentation 7 1. 4-m Upgrades 8 2. Major Instrumentation Efforts 9 3. SOAR 4-m Telescope Project 9 4. CCD Implementation and ARCON Controller Development 10 5. Existing Small General-User Telescopes on Cerro Tololo 10 6. New "Tenant" Installations and Upgrades 10 7. Other 11 B. KPNO 12 1. Image Quality Improvements 12 2. WTYN Queue Observing Experiment 12 3. WTYN 13 4. KPNO Instrumentation Improvements 14 5. Burrell-Schmidt 14 C. NSO 15 1. Kitt Peak 15 2. Sacramento Peak 17 3. Digital Library Development 21 D. USGP/ScOpe 21 E. NOAO Instrumentation 25 1. CCD Mosaic Imager 26 2.
    [Show full text]
  • A Nuclear Molecular Outflow in the Seyfert Galaxy NGC 3227
    Astronomy & Astrophysics manuscript no. ALMANGC3227_final c ESO 2019 June 18, 2019 A nuclear molecular outflow in the Seyfert galaxy NGC 3227 A. Alonso-Herrero1, S. García-Burillo2, M. Pereira-Santaella3, R. I. Davies4, F. Combes5, M. Vestergaard6; 7, S. I. Raimundo6, A. Bunker3, T. Díaz-Santos8, P. Gandhi9, I. García-Bernete10, E. K. S. Hicks11, S. F. Hönig8, L. K. Hunt12, M. Imanishi13; 14, T. Izumi13, N. A. Levenson15, W. Maciejewski16, C. Packham17; 13, C. Ramos Almeida18; 19, C. Ricci8; 20, D. Rigopoulou3, P. F. Roche3, D. Rosario21, M. Schartmann22; 4, A. Usero2, and M. J. Ward21 1 Centro de Astrobiología (CAB, CSIC-INTA), ESAC Campus, E-28692 Villanueva de la Cañada, Madrid, Spain e-mail: [email protected] 2 Observatorio de Madrid, OAN-IGN, Alfonso XII, 3, E-28014 Madrid, Spain 3 Department of Physics, University of Oxford, Keble Road, Oxford OX1 3RH, UK 4 Max Planck Institut für extraterrestrische Physik Postfach 1312, D-85741 Garching bei München, Germany 5 LERMA, Obs. de Paris, PSL Research Univ., Collége de France, CNRS, Sorbonne Univ., UPMC, Paris, France 6 DARK, The Niels Bohr Institute, University of Copenhagen, Vibenshuset, Lyngbyvej 2, DK-2100 Copenhagen O., Denmark 7 Steward Observatory, University of Arizona, 933 N. Cherry Avenue, Tucson, Arizona, USA 8 Núcleo de Astronomía de la Facultad de Ingeniería, Universidad Diego Portales, Av. Ejército Libertador 441, Santiago, Chile 9 Department of Physics & Astronomy, University of Southampton, Hampshire SO17 1BJ, Southampton, UK 10 Instituto de Física de Cantabria, CSIC-Universidad de Cantabria, E-39005 Santander, Spain 11 Department of Physics & Astronomy, University of Alaska Anchorage, AK 99508-4664, USA 12 INAF-Osservatorio Astrofisico di Arcetri, Largo E.
    [Show full text]
  • Astronomy Magazine Special Issue
    γ ι ζ γ δ α κ β κ ε γ β ρ ε ζ υ α φ ψ ω χ α π χ φ γ ω ο ι δ κ α ξ υ λ τ μ β α σ θ ε β σ δ γ ψ λ ω σ η ν θ Aι must-have for all stargazers η δ μ NEW EDITION! ζ λ β ε η κ NGC 6664 NGC 6539 ε τ μ NGC 6712 α υ δ ζ M26 ν NGC 6649 ψ Struve 2325 ζ ξ ATLAS χ α NGC 6604 ξ ο ν ν SCUTUM M16 of the γ SERP β NGC 6605 γ V450 ξ η υ η NGC 6645 M17 φ θ M18 ζ ρ ρ1 π Barnard 92 ο χ σ M25 M24 STARS M23 ν β κ All-in-one introduction ALL NEW MAPS WITH: to the night sky 42,000 more stars (87,000 plotted down to magnitude 8.5) AND 150+ more deep-sky objects (more than 1,200 total) The Eagle Nebula (M16) combines a dark nebula and a star cluster. In 100+ this intense region of star formation, “pillars” form at the boundaries spectacular between hot and cold gas. You’ll find this object on Map 14, a celestial portion of which lies above. photos PLUS: How to observe star clusters, nebulae, and galaxies AS2-CV0610.indd 1 6/10/10 4:17 PM NEW EDITION! AtlAs Tour the night sky of the The staff of Astronomy magazine decided to This atlas presents produce its first star atlas in 2006.
    [Show full text]
  • A Basic Requirement for Studying the Heavens Is Determining Where In
    Abasic requirement for studying the heavens is determining where in the sky things are. To specify sky positions, astronomers have developed several coordinate systems. Each uses a coordinate grid projected on to the celestial sphere, in analogy to the geographic coordinate system used on the surface of the Earth. The coordinate systems differ only in their choice of the fundamental plane, which divides the sky into two equal hemispheres along a great circle (the fundamental plane of the geographic system is the Earth's equator) . Each coordinate system is named for its choice of fundamental plane. The equatorial coordinate system is probably the most widely used celestial coordinate system. It is also the one most closely related to the geographic coordinate system, because they use the same fun­ damental plane and the same poles. The projection of the Earth's equator onto the celestial sphere is called the celestial equator. Similarly, projecting the geographic poles on to the celest ial sphere defines the north and south celestial poles. However, there is an important difference between the equatorial and geographic coordinate systems: the geographic system is fixed to the Earth; it rotates as the Earth does . The equatorial system is fixed to the stars, so it appears to rotate across the sky with the stars, but of course it's really the Earth rotating under the fixed sky. The latitudinal (latitude-like) angle of the equatorial system is called declination (Dec for short) . It measures the angle of an object above or below the celestial equator. The longitud inal angle is called the right ascension (RA for short).
    [Show full text]
  • Observing Galaxies in Pegasus 01 October 2015 23:07
    Observing galaxies in Pegasus 01 October 2015 23:07 Context As you look towards Pegasus you are looking below the galactic plane under the Orion spiral arm of our galaxy. The Perseus-Pisces supercluster wall of galaxies runs through this constellation. It stretches from RA 3h +40 in Perseus to 23h +10 in Pegasus and is around 200 million light years away. It includes the Pegasus I group noted later this document. The constellation is well placed from mid summer to late autumn. Pegasus is a rich constellation for galaxy observing. I have observed 80 galaxies in this constellation. Relatively bright galaxies This section covers the galaxies that were visible with direct vision in my 16 inch or smaller scopes. This list will therefore grow over time as I have not yet viewed all the galaxies in good conditions at maximum altitude in my 16 inch scope! NGC 7331 MAG 9 This is the stand out galaxy of the constellation. It is similar to our milky way. Around it are a number of fainter NGC galaxies. I have seen the brightest one, NGC 7335 in my 10 inch scope with averted vision. I have seen NGC 7331 in my 25 x 100mm binoculars. NGC 7814 - Mag 10 ? Not on observed list ? This is a very lovely oval shaped galaxy. By constellation Page 1 NGC 7332 MAG 11 / NGC 7339 MAG 12 These galaxies are an isolated bound pair about 67 million light years away. NGC 7339 is the fainter of the two galaxies at the eyepiece. I have seen NGC 7332 in my 25 x 100mm binoculars.
    [Show full text]
  • Sejong Open Cluster Survey (SOS)-IV. the Young Open Clusters
    Sejong Open Cluster Survey (SOS) - IV. The Young Open Clusters NGC 1624 and NGC 1931 Beomdu Lim1,5, Hwankyung Sung2, Michael S. Bessell3, Jinyoung S. Kim4, Hyeonoh Hur2, and Byeong-Gon Park1 [email protected] Received ; accepted Not to appear in Nonlearned J., 45. 1Korea Astronomy and Space Science Institute, 776 Daedeokdae-ro, Yuseong-gu, Daejeon 305-348, Korea 2Department of Astronomy and Space Science, Sejong University, 209 Neungdong-ro, arXiv:1502.00105v1 [astro-ph.SR] 31 Jan 2015 Gwangjin-gu, Seoul 143-747, Korea 3Research School of Astronomy and Astrophysics, Australian National University, MSO, Cotter Road, Weston, ACT 2611, Australia 4Steward Observatory, University of Arizona, 933 N. Cherry Ave. Tucson, AZ 85721-0065, USA 5Corresponding author, Korea Research Council of Fundamental Science & Technology Research Fellow –2– ABSTRACT Young open clusters located in the outer Galaxy provide us with an oppor- tunity to study star formation activity in a different environment from the solar neighborhood. We present a UBVI and Hα photometric study of the young open clusters NGC 1624 and NGC 1931 that are situated toward the Galactic anticenter. Various photometric diagrams are used to select the members of the clusters and to determine the fundamental parameters. NGC 1624 and NGC 1931 are, on average, reddened by hE(B − V )i = 0.92 ± 0.05 and 0.74 ± 0.17 mag, respectively. The properties of the reddening toward NGC 1931 indicate an abnormal reddening law (RV,cl = 5.2 ± 0.3). Using the zero-age main se- quence fitting method we confirm that NGC 1624 is 6.0 ± 0.6 kpc away from the Sun, whereas NGC 1931 is at a distance of 2.3 ± 0.2 kpc.
    [Show full text]