DOCSLIB.ORG

Subject Index

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Subject Index Subject Index I. Galaxies kinematics and dynamics, 12, 25, 30, 34, blue compact dwarf (BCD), 4, 14, 33, 67, 79, 82, 86, 87, 129, 138, 139, 39, 56, 57, 81, 175, 185, 189, 208, 155–161, 207, 208, 216, 238, 265, 209, 211, 215, 221–224, 232, 236, 269, 270, 299, 324 237, 241, 243, 253–257, 263, 291, Local Group, 5, 6, 9, 11, 13, 53, 68, 76, 89, 321–324 103, 109, 114, 119, 140, 141, 170, compact elliptical, 135–137 286, 287, 311 low surface brightness (LSB), 134, 136, dark matter (DM), 4, 40, 45, 60, 76, 77, 84, 139, 142, 175, 178–181, 196, 280, 86, 175, 190, 322 287, 296, 311, 317, 318 downsizing, 44, 152–154, 243, 321–324 luminosity function, 135, 141, 186, 187, dwarf elliptical (dE), 7, 60, 76, 82–84, 279, 286, 316, 318 133–143, 155–161, 163–166, 290 Lyman Break, 188, 239, 246 dwarf irregular (dIrr), 4, 8, 15, 25, 33, 43, Lyman continuum escape, 176, 188, 190, 56, 57, 60, 62, 76–82, 84, 85, 103, 200, 239–241 107, 110, 137, 138, 140, 141, 256, Magellanic Clouds (MCs), 27, 51, 52, 62, 261, 263, 291, 296, 299, 301–302 85, 123–127, 170, 171, 180, 311 dwarf spheroidal (dSph), 3–11, 15, 76, morphology and structure, 4–6, 10, 62, 85–89, 95–101, 107, 110, 114, 125, 75–89, 136, 139–141, 156, 164, 130, 134, 141, 143, 185, 311 176–178, 208, 209, 217, 222, 223, 263, 277, 280, 290, 299, 301, 302, formation, 5, 6, 23, 40–43, 55–58, 65–72, 306 75–77, 82, 85, 87, 96–98, 119, nuclei, 66, 68, 70–72, 84, 135, 137, 180, 136, 140, 142, 160, 176, 177, 190, 189 226, 243, 285, 296, 307–310, 318, starburst, 14–15, 27, 28, 30, 32, 33, 60, 76, 321–324 80, 85, 175, 176, 178, 180, 182, green peas, 243–250 184–190, 199, 200, 208, 215, 222, infrared emission, 8, 11, 165, 178, 183, 235–237, 240, 243, 246, 254, 255, 197, 212, 235, 290, 301, 302, 306, 266, 322–324 309 star clusters (SCs), 27, 30, 125, 137, 152, interactions and environmental effects, 5–9, 154, 177, 188, 215, 235–241, 256, 15, 82, 86, 88, 89, 97, 98, 103, 109, 257, 306, 308 114, 136, 138, 165, 166, 177, 185, star formation and feedback processes, 5, 208, 249, 277–279, 281, 286, 287, 6, 12–14, 28, 40, 48, 60, 86, 89, 96, 290, 295, 296, 299, 301, 302, 307, 97, 99, 103, 108, 109, 176, 182, 315, 321–324 185, 208, 248, 249, 306, 308 P. Papaderos et al. (eds.), Dwarf Galaxies: Keys to Galaxy Formation and Evolution, 327 Astrophysics and Space Science Proceedings, DOI 10.1007/978-3-642-22018-0, © Springer-Verlag Berlin Heidelberg 2012 328 Subject Index star formation history (SFH), 4, 9, 12–14, I Zw 123, 223 43, 56, 58, 61, 99, 100, 103–110, II Zw 70, 31, 179, 255 141, 171, 176, 186, 199, 222, 226, J0723C3622, 318 236, 322 J0737C4724, 318 statistics, 43, 45, 96, 134, 137, 196, 200, J0812C4836, 318 238, 239, 245, 318, 322 J0852C1350, 318 surveys, 11, 13, 24, 25, 27, 32, 123, 124, J0926C3343, 318 135, 142, 165, 177, 184, 185, KDG 52, 302 196, 197, 205, 222, 225, 226, 232, KKH 34, 302 236, 246, 261–266, 278–282, 286, Leo A, 5, 103, 105, 106, 256 290–292 Leo I, 135 Tidal Dwarf (TDG), 181, 280, 305–312 Leo II, 135, 287 ultra-compact dwarf, 65–72, 84, 137, 308 LGS3, 9, 103, 105–108, 110, 141 ultra-faint dwarf, 44, 95, 98–100, 134, 142, M32, 136, 137 143, 306 M54, 135 UV emission, 27, 177, 184, 196–202, 231, M82, 31 237–239, 265 Mrk 32, 223 X-ray emission, 15, 24, 28, 30, 78, 79, 83, Mrk 33, 190, 255 190 Mrk 35, 255 Individual Mrk 206, 223, 224 AM 0106-382, 302 Mrk 407, 223 Antlia, 136, 141 Mrk 409, 209, 223, 224 Cetus, 6, 9, 11, 103–109 Mrk 750, 223 CGCG 097-073, 279, 280 Mrk 930, 236 CGCG 097-079, 279, 280 Mrk 1418, 209, 223 DDO 42, 302 NGC 59, 302 DDO 53, 302 NGC 147, 134, 138, 139, 141, 169–172 DDO 68, 318 NGC 185, 134, 138, 139, 141, 165, DDO 82, 302 169–172 DDO 154, 25 NGC 205, 135, 136, 138, 139, 141, 165 DDO 165, 302 NGC 524, 287, 288 DDO 210, 141 NGC 625, 302 Draco, 6, 119–121, 134 NGC 697, 295 ESO 185-13, 236 NGC 891, 269, 270, 286 ESO 215-G009, 141 NGC 1569, 15, 27–32, 79, 81, 254, 302 ESO 245-G005, 302 NGC 1705, 79 ESO 347-G017, 302 NGC 2419, 135 ESO 348-G009, 302 NGC 3077, 28, 29 ESO 473-G024, 302 NGC 3738, 302 ESO 338-04, 179, 188, 237, 238 NGC 3741, 25 Fornax, 66, 71, 134, 138 NGC 4013, 286 Haro 2, 27, 29, 255 NGC 4214, 27, 29, 30, 254 Haro 3, 255 NGC 4449, 27, 28, 30–33, 79 Haro 11, 180, 188, 190, 236 NGC 4630, 181 He 2-10, 27, 30, 79, 232 NGC 5033, 295 Holmberg II, 13, 50, 51 NGC 5128, 135 IC 10, 180, 266 NGC 5253, 30, 79, 215–218 IC 65, 295, 296 NGC 5291, 309 IC 1613, 103, 105, 109 NGC 5846A, 136, 137 IC 2574, 13 NGC 6278, 295 IC 3328, 7, 139 NGC 6456, 179, 186 IC 4318, 85 NGC 6822, 177, 180, 256 I Zw 18, 28, 40, 44, 45, 79, 179, 182, NGC 6962, 295, 299 183, 254, 256, 322 Phoenix, 9, 103–105, 107, 141 Subject Index 329 Sagittarius, 113–116, 142, 143 M81, 13, 301, 302 SAO 0822C3545, 318 Sculptor, 8, 301 SBS 0335-052, 178, 182, 183, 238, 239, 322 Sculptor, 53, 54, 98–100, 134 Sextans B, 53, 256 V. S t a r s Tol 1432C032, 223, 224 abundances, 5, 8, 9, 52–54, 59–63, 82, Tol 1924-416, 179, 209, 210 84, 86, 87, 89, 96–100, 120, 121, Tucana, 6, 9, 11, 103–109, 287 127–130, 141–143, 158, 160, 161 UGC 4483, 302 asymptotic giant branch (AGB), 127, 170 UGCA 442, 302 carbon, 4, 124, 125 Ursa Minor, 135 Hertzsprung-Russell and C-M diagrams, VCC 209, 165, 166 8, 13, 40, 103–105, 107, 124, 177, VCC 523, 156, 157, 159 185, 256, 298 VCC 562, 291 initial mass function (IMF), 9–10, 13, VCC 781, 165, 166 151–154, 176, 189, 198, 200, 201, VCC 951, 165, 166 208, 256 VCC 1087, 139, 156, 157, 159 long period variables (LPVs), 169–172 VCC 1179, 291 red giant branch (RGB), 30, 170 VCC 1217, 85 Wolf-Rayet, 14, 207, 208, 216, 222, VCC 1261, 139, 156, 157, 159 231–234 VCC 1356, 291 Individual VCC 1627, 136 Fehrenbach-Duflot, 127–130 VCC 1861, 159 VCC 2062, 309 VI. Interstellar medium (ISM) II. Cosmology abundances, 11, 12, 15, 24, 26, 57, 58, dark ages, reionization, first stars, 10, 11, 77, 79–81, 175, 180–183, 208, 44, 77, 86, 95, 96, 103–110 222, 226–228, 232, 233, 244–249, early Universe, 10, 11, 23, 34, 40, 82, 86, 253–257, 280–282, 286, 322 89, 103, 244, 310 atomic hydrogen (HI), 12–14, 24–26, 30, 45, 48–52, 62, 78, 79, 141, 165, 166, 177, 178, 180, 202, 263, 265, III. Galaxy Clusters 266, 269–272, 291, 307, 310 Individual bubbles and supernova remnants, 15, 79, Abell 539, 281, 282 254, 323 Abell 634, 281, 282 dust content and dust extinction, 24, 26, Abell 1367, 279, 280 140, 163–166, 180, 183, 197, 199, Abell 2151, 280, 281 207, 208, 216, 223, 224, 226, 237, Coma, 32, 82, 84, 279, 296 240, 278, 289–292 Fornax, 67, 82, 84, 136, 137, 278, 296, gaseous halos, 15, 27, 30, 32, 33, 86, 188, 298 190, 269, 270, 278, 322, 324 Hercules, 279, 280 HII regions, 8, 24, 27, 30, 77, 81, 182, 200, Hydra, 279 207, 215–218, 222, 224, 269–272, Virgo, 7, 68, 70, 71, 76, 82–85, 278, 316 135–141, 155–161, 164–166, 278, magnetic fields, 24, 31, 32 279, 289–292, 296, 298, 309 molecular gas, 11, 12, 24, 26–28, 44, 97, 165, 166, 180, 181, 184, 190, 263–265, 306, 309 IV. Galaxy Groups structure and kinematics, 12, 13, 25, 26, 30, Individual 34, 52, 62, 78–80, 83, 85, 177, 178, Cen A, 141, 215 208, 209, 238, 263, 265, 269–271, IC 342, 30 324 330 Subject Index VII. Techniques VIII. Telescopes evolutionary synthesis, 232, 233, 250 Calar Alto 1.23m, 296 Calar Alto 3.5m, 208, 270 hydrodynamical simulations, 48, 60, 65, CFHT, 311 78, 79, 86, 120, 257, 309, 311 CHANDRA, 24, 28, 30 integral field spectroscopy (IFS), 156, GAIA, 123 205–212, 221–224, 270, 309 GALEX, 8, 11, 177, 183, 190, 196, 197, N-body/SPH simulations, 40, 45, 48–52, 238, 263, 306 60–62, 66–71, 87, 89, 114, 115, Gran Telescopio Canarias (GTC), 250 136, 307–310 HERSCHEL, 12, 140, 156, 164–166, 180, photometric, 12, 104, 123, 135–138, 157, 190, 264, 265, 290, 291 161, 170, 226, 295–299, 315–319 Hubble Space Telescope, 4, 10, 12–14, 40, semi-analytical, 45, 151, 257 104, 136, 177, 190, 216, 235–237 LOFAR, 24, 32, 33, 190, 323 spectral synthesis, 128, 208, 211, 225, 236 SPITZER, 11, 12, 177, 190, 196–198, 263, spectroscopic, 128, 138, 139, 190, 306 205–212, 216, 221–224, 244, 250, VLA, 12, 24, 25, 177, 263–265 296, 309, 316 VLT, 208, 209, 212, 216, 222, 239, 240 surface photometry, 296, 302 WIYN 0.9m, 286 Author Index Aaronson, M., 4 Atek, H., 238, 240 Abazajian, K.N., 232 Azzopardi, M., 124 Abbott, D.C., 231 Abel, T., 10, 49, 50 Adamo, A., 188, 236, 238 Baade, W., 134 Adelberger, K.L., 97, 246, 249 Babul, A., 10, 78 Adelman-McCarthy, J.K., 232 Bacon, R., 156–158, 161, 206, 207, 212 Aden,´ D., 142 Baes, M., 140, 163–166, 289–292 Agertz, O., 309 Bagetakos, I., 26 Agiienko, K., 161, 231–233 Bagnuolo, W.G., 183, 189 Aguerri, J.A.L., 255, 256, 296 Baker, A.J., 27 Ajhar, E.A., 60, 136, 138, 158 Baker, A.L., 12, 182, 184 Akiyama, S., 197, 198, 200 Balcells, M., 158 Alard, C., 157, 170 Baldry, I.K., 43, 45 Alcock, C., 130, 170 Baldwin, J.A., 217, 226 Allen, D.A., 232 Balkowski, C., 309 Balogh, M., 278 Allen, R.J., 270 Barazza, F.D., 60, 138–140, 296, 298, 299 Allsman, R.A., 170 Bardalez-Gagliuffi, D.C., 286 Aloisi, A., 40, 183 Barentine, J.C., 286 Altschuler, D.R., 31 Barkana, R., 77 Amor´ın, R.O., 243–250, 254, 256 Barnes, D.G., 25, 177 Amram, P., 188, 241, 306, 309 Barnes, J.E., 307, 309 Andersson, B., 200 Barone, L.T., 27 Anelli, D., 78 Bastian, N., 13 Angeretti, L., 79 Bauer, F.E., 28 Aparicio, A., 9, 13, 106, 256 Bauer, S.M., 270 Appleton, P.N., 306 Beasley, M.A., 139, 157, 161 Aragon-Salamanca,´ A., 158 Beaton, R.L., 178, 286 Ardeberg, A., 121 Beck, R., 31 Armus, L., 189 Beck, T.L., 137 Arnberg, D., 200 Becker, R.H., 107 Arnouts, S., 296 Becker, T., 206, 270 Asari, N.V., 228 Beers, T.C., 129 Ascasibar, Y., 55–58 Begum, A., 12, 25, 26, 177, 178, 182, 322 Asplund, M., 181 Beierle, M.E., 25 P.
Load more

Recommended publications
  • The Violent ISM in Haro 11
    Stockholm University Department of Astronomy LICENTIATE THESIS The violent ISM in Haro 11 Author: Veronica Menacho Menacho Department of Astronomy, The Oskar Klein Center, Stockholm University, AlbaNova, 106 91 Stockholm, Sweden Supervisor: Goran¨ Ostlin¨ Co-Supervisor: Arjan Bik January 10, 2019 Abstract This thesis introduces briefly physical processes operating in the ISM around massive stars and focuses on the impact strong stellar feedback has in creating large-scale structures in a galaxy. Stellar feedback is ubiquitous in star forming galaxies and its effect on the ISM depends strongly on the energy output from the most massive stars (M≥7 M ) and the properties of the surrounding gas. Starburst galaxies are among the most active in producing large amount of massive star clusters with stellar populations up to thousands of massive stars. In the first 4 Myr of the star clusters evolution, radiative feedback of the most massive stars (M≥30 M ) are at work. Large amount of ionizing photons are released to the ambient medium while radiative pressure compress the surrounding gas. At the same time their stellar winds inject continuously mechanical energy and momentum in their surrounding. This mechanical feedback is then at later ages, until ∼ 40 Myrs, maintained by supernova explosions from the less massive stars. Strong stellar feedback tends to develop large-scale structures such as bubbles, loops, fil- aments and outflows. These are transient structures and can be seen as imprints of how the released energy is clearing or has cleared paths in the ISM. Strong stellar feedback can have devastating consequences in dwarf galaxies due to their shallow gravitational potential.
    [Show full text]
  • Arxiv:1704.01678V2 [Astro-Ph.GA] 28 Jul 2017 Been Notoriously Difficult, Resulting Mostly in Upper Lim- Highest Escape Fractions Measured to Date Among Low- Its (E.G
    Submitted: 3 March 2017 Preprint typeset using LATEX style AASTeX6 v. 1.0 MRK 71 / NGC 2366: THE NEAREST GREEN PEA ANALOG Genoveva Micheva1, M. S. Oey1, Anne E. Jaskot2, and Bethan L. James3 (Accepted 24 July 2017) 1University of Michigan, 311 West Hall, 1085 S. University Ave, Ann Arbor, MI 48109-1107, USA 2Department of Astronomy, Smith College, Northampton, MA 01063, USA 3STScI, 3700 San Martin Drive, Baltimore, MD 21218, USA ABSTRACT We present the remarkable discovery that the dwarf irregular galaxy NGC 2366 is an excellent analog of the Green Pea (GP) galaxies, which are characterized by extremely high ionization parameters. The similarities are driven predominantly by the giant H II region Markarian 71 (Mrk 71). We compare the system with GPs in terms of morphology, excitation properties, specific star-formation rate, kinematics, absorption of low-ionization species, reddening, and chemical abundance, and find consistencies throughout. Since extreme GPs are associated with both candidate and confirmed Lyman continuum (LyC) emitters, Mrk 71/NGC 2366 is thus also a good candidate for LyC escape. The spatially resolved data for this object show a superbubble blowout generated by mechanical feedback from one of its two super star clusters (SSCs), Knot B, while the extreme ionization properties are driven by the . 1 Myr-old, enshrouded SSC Knot A, which has ∼ 10 times higher ionizing luminosity. Very massive stars (> 100 M ) may be present in this remarkable object. Ionization-parameter mapping indicates the blowout region is optically thin in the LyC, and the general properties also suggest LyC escape in the line of sight.
    [Show full text]
  • The Molecular Gas Reservoir of 6 Low-Metallicity Galaxies from the Herschel Dwarf Galaxy Survey a Ground-Based Follow-Up Survey of CO(1–0), CO(2–1), and CO(3–2)
    A&A 564, A121 (2014) Astronomy DOI: 10.1051/0004-6361/201322096 & c ESO 2014 Astrophysics The molecular gas reservoir of 6 low-metallicity galaxies from the Herschel Dwarf Galaxy Survey A ground-based follow-up survey of CO(1–0), CO(2–1), and CO(3–2) D. Cormier1,S.C.Madden2, V. Lebouteiller2,S.Hony3, S. Aalto4, F. Costagliola4,5, A. Hughes3, A. Rémy-Ruyer2, N. Abel6, E. Bayet7, F. Bigiel1, J. M. Cannon8,R.J.Cumming9, M. Galametz10, F. Galliano2, S. Viti11,andR.Wu2 1 Institut für theoretische Astrophysik, Zentrum für Astronomie der Universität Heidelberg, Albert-Ueberle Str. 2, 69120 Heidelberg, Germany e-mail: [email protected] 2 Laboratoire AIM, CEA/DSM – CNRS – Université Paris Diderot, Irfu/Service d’Astrophysique, CEA Saclay, 91191 Gif-sur-Yvette, France 3 Max-Planck-Institute for Astronomy, Königstuhl 17, 69117 Heidelberg, Germany 4 Department of Earth and Space Sciences, Chalmers University of Technology, Onsala Space Observatory, 439 92 Onsala, Sweden 5 Instituto de Astrofísica de Andalucía, Glorieta de la Astronomía s/n, 18008 Granada, Spain 6 University of Cincinnati, Clermont College, Batavia OH 45103, USA 7 Sub-Dept. of Astrophysics, Dept. of Physics at University of Oxford, Denys Wilkinson Building, Keble Road, Oxford OX1 3RH, UK 8 Department of Physics & Astronomy, Macalester College, 1600 Grand Avenue, Saint Paul MN 55105, USA 9 Onsala Space Observatory, Chalmers University of Technology, 439 92 Onsala, Sweden 10 Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK 11 Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, UK Received 17 June 2013 / Accepted 17 November 2013 ABSTRACT Context.
    [Show full text]
  • Space Telescope Science Institute Investigators Title
    PROP ID: 16100 Principal Investigator: Julia Roman-Duval PI Institution: Space Telescope Science Institute Investigators Title: ULLYSES SMC O7-O9 Giants COS Cycle: 27 Allocation: 8 orbits Proprietary Period: 0 months Program Status: Program Coordinator: Tricia Royle Visit Status Information None PROP ID: 16101 Principal Investigator: Julia Roman-Duval PI Institution: Space Telescope Science Institute Investigators Title: ULLYSES SMC B1 Stars COS Cycle: 27 Allocation: 12 orbits Proprietary Period: 0 months Program Status: Program Coordinator: Tricia Royle Visit Status Information None PROP ID: 16102 Principal Investigator: Julia Roman-Duval PI Institution: Space Telescope Science Institute Investigators Title: SMC B2 to B4 Supergiants COS/STIS Cycle: 27 Allocation: 16 orbits Proprietary Period: 0 months Program Status: Program Coordinator: Tricia Royle Contact Scientist: Sergio Dieterich Visit Status Information None PROP ID: 16103 Principal Investigator: Julia Roman-Duval PI Institution: Space Telescope Science Institute Investigators Title: ULLYSES SMC O Stars COS 1096 Cycle: 27 Allocation: 17 orbits Proprietary Period: 0 months Program Status: Program Coordinator: Tricia Royle Contact Scientist: Julia Roman-Duval Visit Status Information None PROP ID: 16104 Principal Investigator: Julia Roman-Duval PI Institution: Space Telescope Science Institute Investigators Title: ULLYSES UV Pre-imaging of Sextans A and NGC 3109 Targets Cycle: 27 Allocation: 2 orbits Proprietary Period: 0 months Program Status: Program Coordinator: Tricia Royle Visit
    [Show full text]
  • Cycle 25 Approved Programs
    Cycle 25 Approved Programs Phase II First Name Last Name Institution Country Type Resources Title 15328 Jessica Agarwal Max Planck Institute for Solar DEU GO 5 Orbital period and formation process of the exceptional binary asteroid System Research system 288P 15090 Marcel Agueros Columbia University in the City of USA GO 35 A UV spectroscopic survey of periodic M dwarfs in the Hyades New York 15091 Marcel Agueros Columbia University in the City of USA SNAP 86 A UV spectroscopic snapshot survey of low-mass stars in the Hyades New York 15092 Monique Aller Georgia Southern University Res. USA GO 6 Testing Dust Models at Moderate Redshift: Is the z=0.437 DLA toward 3C & Svc. Foundation, Inc 196 Rich in Carbonaceous Dust? 15193 Alessandra Aloisi Space Telescope Science Institute USA GO 22 Addressing Ionization and Depletion in the ISM of Nearby Star-Forming Galaxies 15194 Alessandra Aloisi Space Telescope Science Institute USA GO 18 The Epoch of the First Star Formation in the Closest Metal-Poor Blue Compact Dwarf Galaxy UGC 4483 15299 Julian Alvarado GomeZ Smithsonian Institution USA GO 13 Weaving the history of the solar wind with magnetic field lines Astrophysical Observatory 15093 Jennifer Andrews University of Arizona USA GO 18 Dwarfs and Giants: Massive Stars in Little Dwarf Galaxies 15222 Iair Arcavi University of California - Santa USA GO 1 What Type of Star Made the One-of-a-kind Supernova iPTF14hls? Barbara 15223 Matthew Auger University of Cambridge GBR GO 1 The Brightest Galaxy-Scale Lens 15300 Thomas Ayres University of Colorado
    [Show full text]
  • Kinematics of Haro 11: the Miniature Antennae? G
    A&A 583, A55 (2015) Astronomy DOI: 10.1051/0004-6361/201323233 & c ESO 2015 Astrophysics Kinematics of Haro 11: The miniature Antennae? G. Östlin1, T. Marquart2;1, R. J. Cumming3, K. Fathi1, N. Bergvall2, A. Adamo1, P. Amram4, and M. Hayes1 1 Oskar Klein Centre, Department of Astronomy, Stockholm University, 106 91 Stockholm, Sweden e-mail: [email protected] 2 Department of Physics and Astronomy, Uppsala University, Box 515, 751 20 Uppsala, Sweden 3 Onsala Space Observatory, Chalmers University of Technology, 43992 Onsala, Sweden 4 Aix-Marseille Université, CNRS, LAM (Laboratoire d’Astrophysique de Marseille), 13388 Marseille, France Received 11 December 2013 / Accepted 27 July 2015 ABSTRACT Luminous blue compact galaxies are among the most active galaxies in the local Universe in terms of their star formation rate per unit mass. They are rare at the current cosmic epoch, but were more abundant in the past and may be seen as the local analogues of higher red shift Lyman break galaxies. Studies of their kinematics is key to understanding what triggers their unusually active star formation. In this work, we investigate the kinematics of stars and ionised gas in Haro 11, one of the most luminous blue compact galaxies in the local Universe. Previous works have indicated that many of these galaxies may be triggered by galaxy mergers. We have employed Fabry-Perot interferometry, long-slit spectroscopy, and integral field unit (IFU) spectroscopy to explore the kinematics of Haro 11. We target the near-infrared calcium triplet, and use cross-correlation and penalised pixel fitting techniques to derive the stellar velocity field and velocity dispersion.
    [Show full text]
  • Report of Contributions
    How Galaxies form Stars Report of Contributions https://indico.fysik.su.se/e/5696 How Galaxies for … / Report of Contributions Opening Remarks, Setting the Stag … Contribution ID: 319 Type: not specified Opening Remarks, Setting the Stage (I) Monday, 22 August 2016 09:10 (35 minutes) Presenter: ÖSTLIN, Göran (Stockholm University) September 30, 2021 Page 1 How Galaxies for … / Report of Contributions Challenges and first results from C … Contribution ID: 381 Type: not specified Challenges and first results from CO and IR measurements in local Lyman Alpha Emitters Friday, 26 August 2016 14:10 (20 minutes) Carbon Monoxide has proven to be a well-calibrated tracer of the total molecular gas content in galaxies at low and high redshift. However, CO observations in galaxies of subsolar metallicity remain challenging, even in the local universe. For that reason, the dust mass is often used to infer the molecular gas in low metallicity systems. I will present first results of CO and dust measurements in the Lyman Alpha Reference Sample (LARS), a sample of local Lyman Alpha emitting starburst galaxies, all of subsolar metallicity. Using multiple-J CO transitians obtained with APEX and the IRAM 30m telescope, as well as Herschel/PACS and WISE data in combination with physical dust models and PDR codes, properties of the star forming gas could be derived and CO and dust scaling relations studied. Primary author: PUSCHNIG, Johannes (Stockholm University) Presenter: PUSCHNIG, Johannes (Stockholm University) Session Classification: Global Properties at Low and High Redshifts (continuation) September 30, 2021 Page 2 How Galaxies for … / Report of Contributions Beyond turbulence: a fundamenta … Contribution ID: 382 Type: not specified Beyond turbulence: a fundamentally different mode of star formation in Orion We argue that Orion hosts a fundamentally different mode of star cluster formation relative to the nearby clouds (e.g., Taurus) that have been studied to death.
    [Show full text]
  • Stsci Newsletter: 2017 Volume 034 Issue 02
    2017 - Volume 34 - Issue 02 Emerging Technologies: Bringing the James Webb Space Telescope to the World Like the rest of the Institute, excitement is building in the Office of Public Outreach (OPO) as the clock winds down for the launch of the James Webb Space Telescope. Our task is translating and sharing this excitement over groundbreaking engineering—and the scientific discoveries to come—with the public. Webb @ STScI In the lead-up to Webb’s launch in Spring 2019, the Institute continues its work as the science and operations center for the mission. The Institute has played a critical role in a number of recent Webb mission milestones. Updates on Hubble Operation at the Institute Observations with the Hubble Space Telescope continue to be in great demand. This article discusses Cycle 24 observing programs and scheduling efficiency, maintaining COS productivity into the next decade, keeping Hubble operations smooth and efficient, and ensuring the freshness of Hubble archive data. Hubble Cycle 25 Proposal Selection Hubble is in high demand and continues to add to our understanding of the universe. The peer-review proposal selection process plays a fundamental role in establishing a merit-based science program, and that is only possible thanks to the work and integrity of all the Time Allocation Committee (TAC) and review panel members, and the external reviewers. We present here the highlights of the Cycle 25 selection process. Using Gravity to Measure the Mass of a Star In a reprise of the famous 1919 solar eclipse experiment that confirmed Einstein's general relativity, the nearby white dwarf, Stein 2051 B, passed very close to a background star in March 2014.
    [Show full text]
  • Book of Abstracts
    How Galaxies form Stars Monday 22 August 2016 - Friday 26 August 2016 AlbaNova University Center, Stockholm University, Stockholm, Sweden Book of Abstracts Contents Opening Remarks, Setting the Stage (I) ............................ 1 Challenges and first results from CO and IR measurements in local Lyman Alpha Emitters 1 Beyond turbulence: a fundamentally different mode of star formation in Orion . 1 Superbubbles, Supernovae, and Deregulating Galaxies: Too Big Not to Fail . 2 The outer filaments of Centaurus A .............................. 2 Simulations of realistic dwarf galaxies including Population III feedback . 3 Blustering and Blasting - Stellar feedback and its Chemical Tracers ............ 4 The Hierarchical Distribution of Young Stellar Clusters in Nearby Galaxies . 4 Characterizing Dust Attenuation in Local Star Forming Galaxies .............. 5 Constraining the cloud-scale physics of star formation and feedback in galaxies across cos- mic time ........................................... 5 How black hole feedback may trigger star formation in galaxies .............. 6 Star Formation in the outer M83 XUV disk .......................... 6 Star Formation and Feedback in Low Metallicity Galaxies at z~2 .............. 7 The impact of galactic environment on star formation .................... 7 Theory of star formation and feedback (I) ........................... 8 The effect of galaxy dynamics on star formation (I) ..................... 8 The Gas-Star Cycle resolved from Galactic to Cloud Scale in Nearby Galaxies . 9 Synthetic observations of star formation tracers in disc galaxy simulations — the validation of a new method to constrain the cloud-scale physics of star formation and feedback 9 [CII] as a tracer of GMC formation .............................. 10 Cold gas and star formation on clump scales: an ALMA look at a prototypical z~2 galaxy 10 Triggered formation of cold gas from superbubbles ....................
    [Show full text]
  • Andrea Heather Prestwich - Curriculum Vitae
    Andrea Heather Prestwich - Curriculum Vitae Born: 1 April 1962, Bristol, England Citizenship: United States Education: • Ph.D. in Astrophysics, Imperial College, London (1989) • M.Sc in Radio Astronomy, Univerity of Manchester (1985) • B.Sc. (Hons) in Physics, Queen Mary College, London (1984) Employment: March 2014 - present Team Lead, Chandra Peer Review March 2010 - March 2014 Coordinator, NASA Einstein Postdoctoral Fellowship Program March 2000 - present Astrophysicist, Chandra Director's Office, CXC January 1995 - Feb 2000 Astrophysicist, Chandra Users' Support Group, CXC January 1992 - January 1995 Einstein Data Center Archive Scientist, SAO December 1989-December 1991 NRC Post-doctoral Research Associate, NASA-MSFC September 1988-June 1989 Lecturer, Harvard University October 1985-1988 Graduate Student, Imperial College, London Mentoring and Student Supervision: December 2013 - present Member Thesis Committee Matthew Brorby, University of Iowa May 2012 - July 2012 Member Thesis Committee Blagoy Rangelov, University of Toledo March 2012 - March 2013 Supervised SAO predoc Floyd Jackson Sept - Dec 2010 Supervised SAO predoc Floyd Jackson May 2008 - May 2011 Supervised SAO predoc Blagoy Rangelov Sept 2003-Sept 2007 Co-supervised PhD work of Roy Kilgard Professional Societies • Fellow of Royal Astronomical Society • Member of American Astronomical Society Invited Talks • May 2011, Ultra-Luminous X-ray Sources in the Most Metal Poor galaxies, invited talk at AAS topical session • December 2009, Center for Astrophysics Observatory Night
    [Show full text]
  • 230Th AAS Session Table of Contents
    230th AAS Austin, TX – June, 2017 Meeting Abstracts Session Table of Contents 100 – Welcome Address by AAS President Christine Jones (Harvard-Smithsonian, CfA) 101 – Kavli Foundation Lecture: Dark Matter in the Universe, Katherine Freese (University of Michigan) 102 – Extrasolar Planets: Detection and Future Prospects 103 – Instrumentation, and Things to do with Instrumentation: From the Ground 104 – Topics in Astrostatistics 105 – Inner Solar Systems: Planet Compositions as Tracers of Formation Location 106 – Annie Jump Cannon Award: Origins of Inner Solar Systems, Rebekah Dawson (Penn State University) 108 – Astronomy Education: Research, Practice, and Outreach Across the Human Continuum 109 – Bridging Laboratory & Astrophysics: Atomic Physics 110 – Preparing for JWST Observations: Insights from First Light and Assembly of Galaxies GTO Programs I 111 – Inner Solar Systems: Super-Earth Orbital Properties: Nature vs. Nurture 112 – Plenary Talk: The Universe's Most Extreme Star-forming Galaxies, Caitlin Casey (University of Texas, Austin) 113 – Plenary Talk: Science Highlights from SOFIA, Erick Young (USRA) 114 – Preparing for JWST Observations Poster Session 115 – Astronomy Education: Research, Practice, and Outreach Across the Human Continuum Poster Session 116 – Societal Matters Poster Session 117 – Instrumentation Poster Session 118 – Extrasolar Planets Poster Session 119 – The Solar System Poster Session 200 – LAD Plenary Talk: The Rosetta Mission to Comet 67P/ Churyumov-Gerasimenko, Bonnie Buratti (JPL) 201 –
    [Show full text]
  • ASTRONOMY and ASTROPHYSICS REVIEW the Most Metal-Poor
    The Astron Astrophys Rev (2000) 10: 1–79 THE Digital Object Identifier (DOI) 10.1007/s001590000005 ASTRONOMY AND ASTROPHYSICS The most metal-poor galaxies REVIEW D. Kunth?,G.Ostlin¨ ?? Institut d’Astrophysique de Paris (IAP), 98bis Boulevard Arago, 75014 Paris, France Received 19 August 1999 / Published online: 15 February 2000 – c Springer-Verlag 2000 Abstract. Metallicity is a key parameter that controls many aspects in the formation and evolution of stars and galaxies. In this review we focus on the metal deficient galaxies, in particular the most metal-poor ones, because they play a crucial roleˆ in the cosmic scenery. We first set the stage by discussing the difficult problem of defining a global metallicity and how this quantity can be measured for a given galaxy. The mechanisms that control the metallicity in a galaxy are reviewed in detail and involve many aspects of modern astrophysics: galaxy formation and evolution, massive star formation, stellar winds, chemical yields, outflows and inflows etc. Because metallicity roughly scales as the galactic mass, it is among the dwarfs that the most metal-poor galaxies are found. The core of our paper reviews the considerable progress made in our understanding of the properties and the physical processes that are at work in these objects. The question on how they are related and may evolve from one class of objects to another is discussed. While discussing metal-poor galaxies in general, we present a more detailed discussion of a few very metal-poor blue compact dwarf galaxies like IZw18. Although most of what is known relates to our local universe, we show that it pertains to our quest for primeval galaxies and is connected to the question of the origin of structure in the universe.
    [Show full text]