DOCSLIB.ORG

Appendix for Ref. 26 of “Modern Cosmology: Interactive Computer Simulations That Use Recent Observational Surveys”

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Appendix for Ref. 26 of “Modern Cosmology: Interactive Computer Simulations That Use Recent Observational Surveys” Appendix for Ref. 26 of \Modern Cosmology: Interactive Computer Simulations that use Recent Observational Surveys" Jacob Moldenhauer1∗, Larry Engelhardt1, Keenan M. Stone1, Ezekiel Shuler1 1Department of Physics and Astronomy, Francis Marion University, Florence, SC 29506, USA; (Dated: February 4, 2013) 1 A. G. Riess et al., \Type Ia Supernova Discoveries at z > 1 from the Hubble Space Telescope: Evidence for Past Deceleration and Constraints on Dark Enenrgy Evolution", Astrophys. J., 607, 665 (2004); A.G. Riess et al., \New Hubble Space Telescope Discoveries of Type Ia Supernovae at z > 1: Narrowing Constraints on the Early Behavior of Dark Energy", Astrophys. J. 659, 98 (2007). 2 P. Astier et al., \The Supernova Legacy Survey: Measurement of Ωm,ΩΛ and w from the First Year Data Set", Astron. As- trophys., 447, 31 (2006). 3 T. Davis et al., \Scrutinizing Exotic Cosmological Models Using ESSENCE Supernova Data Combined with Other Cosmo- logical Probes", Astrophys. J. 666, 716 (2007). 4 M. Kowalski et al., \Improved Cosmological Constraints from New, Old and Combined Supernova Datasets", Astrophys. J. 686, 749 (2008); Union data sets include M. Hamuy, et al., \The Absolute Luminosities of the Calan/Tololo Type Ia Supernovae", Astron. J., 112, 2408 (1996); K. Krisciunas et al., \Optical and Infrared Photometry of the Nearby Type Ia Supernovae 1999ee, 2000bh, 2000ca, and 2001ba", Astron. J., 127, 1664 (2004a), K. Krisciunas et al.,\Optical and Infrared Photometry of the Type Ia Supernovae 1991T, 1991bg, 1999ek, 2001bt, 2001cn, 2001cz, and 2002bo", Astron. J., 128, 3034 (2004b), K. Krisciunas et al.,\Optical and Infrared Photometry of the Type Ia Supernovae 1999da, 1999dk, 1999gp, 2000bk, and 2000ce", Astron. J., 122, 1616 (2001); A. G. Riess et al., `Observational Evidence from Supernovae for an Acclerating Universe and a Cosmological Constant", Astron. J., 116, 1009 (1998), A. G. Riess et al., \BVRI Light Curves for 22 Type Ia Supernovae", Astron. J., 117, 707 (1999), A. G. Riess et al., \Type Ia Supernova Discoveries at z > 1 from the Hubble Space Telescope: Evidence for Past Deceleration and Constraints on Dark Enenrgy Evolution", Astrophys. J., 607, 665 (2004); A.G. Riess et al., \New Hubble Space Telescope Discoveries of Type Ia Supernovae at z > 1: Narrowing Constraints on the Early Behavior of Dark Energy", Astrophys. J. 659, 98 (2007). S. Jha et al., \UBVRI Light Curves of 44 Type Ia Supernovae", Astron. J., 131, 527 (2006), S. Jha et al., \Improved Distances to Type Ia Supernovae with Multicolor Light Curve Shapes: MLCS2k2", Astrophys. J., 659, 122 (2007); Perlmutter et al., \Measurements of Omega and Lambda from 42 High-Redshift Supernovae", Astrophys. J., 517, 565 (1999); J. L. Tonry et al., \Cosmological Results from High-z Supernovae", Astrophys. J., 594, 1 (2003); B. J. Barris et al., \23 High Redshift Supernovae from the IfA Deep Survey: Doubling the SN Sample at z>0.7", Astrophys. J., 602, 571 (2004); R. A. Knop et al., \New Constraints on M , , and w from an Independent Set of Eleven High-Redshift Supernovae Observed with HST", Astrophys. J., 598, 102 (2003); P. Astier et al., \The Supernova Legacy Survey: Measurement of Ωm,ΩΛ and w from the First Year Data Set", Astron. Astrophys., 447, 31 (2006); G. Miknaitis et al., \The ESSENCE Supernova Survey: Survey Optimization, Observations, and Supernova Photometry", Astrophys. J., 666, 674 (2007); W. M. Wood-Vasey et al., Astrophys. J., \Observational Constraints on the Nature of the Dark Energy: First Cosmological Results from the ESSENCE Supernova Survey", 666, 694 (2007); P. M. Garnavich et al., \Supernova Limits on the Cosmic Equation of State", Astrophys. J., 509, 74 (1998); B. P. Schmidt et al., \The High-Z Supernova Search: Measuring Cosmic Deceleration and Global Curvature of the Universe Using Type Ia Supernovae", Astrophys. J., 507, 46 (1998). 5 M. Hicken et al., \CfA3: 185 Type Ia Supernova Light Curves from the CfA", Astrophys. J., 700, 1097 (2009). 6 R. Amanullah et al., \Spectra and Light Curves of Six Type Ia Supernovae at 0:511 < z < 1:12 and the Union2 Compilation", Astrophys. J. 716, 712 (2010), arXiv:1004.1711. 7 N. Suzuki et al., \The Hubble Space Telescope Cluster Supernova Survey: V. Improving the Dark Energy Constraints Above z>1 and Building an Early-Type-Hosted Supernova Sample", ApJ Dec. 20, (2011). 8 H. Wei, \Observational Constraints on Cosmological Models with the Updated Long Gamma-Ray Bursts", J. Cosmol. As- tropart. Phys.JCAP1008:020, (2010). 9 D. Stern, R. Jimenez, L. Verde, M. Kamionkowski, S. A. Stanford, \Cosmic Chronometers: Constraining the Equation of State of Dark Energy. I: H(z) Measurements", J. Cosmol. Astropart. Phys., JCAP02(2010)008. 10 E. Gaztanaga, A. Cabre, L. Hui, \Clustering of Luminous Red Galaxies IV: Baryon Acoustic Peak in the Line-of-Sight Direction and a Direct Measurement of H(z)", Mon. Not. R. Astron. Soc., 399, 1663 (2009). 11 B. A. Reid, et al., \The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: measurements of the growth of structure and expansion rate at z = 0:57 from anisotropic clustering", submitted Mon. Not. R. Astron. Soc., ∗ Electronic address: [email protected] 2 TABLE I: Table I: Table of Observational Surveys we include for CosmoEJS. We list the Observational Survey Name (Type), Number in Survey, Redshift (z) Range, Description of the Survey, Parameters To Fit, Filename, Format of the data sets. Survey Name Number Redshift (z) Description of the Survey Parameters Filename Format (Type) in Survey Range To Fit 2004 release of 186 supernovae including the Riess 186 0.01 ! 1.755 "gold" sample of 157 supernovae and additional Ωm,ΩΛ,Ωk sn data riess.txt (z; µ(z); σ) 1 (SNe) "silver" by which includes other older datasets. H0, w0, wa Supernovae Legacy Survey Collaboration of 115 SNLS I 115 0.05 ! 1.01 supernovae including 71 from the first year Ωm,ΩΛ,Ωk snls.txt (z; µ(z); σ) 2 (SNe) SNLS and others by . H0, w0, wa Compilation of 192 supernovae by3 Davis 192 0.016 ! 1.755 including supernoave from ESSENCE Survey Ωm,ΩΛ,Ωk DavisSN2007data.txt (z; µ(z); σ) (SNe) and other older sets. H0, w0, wa The Supernova Cosmology Project (SCP) Union Union 307 0.015 ! 1.551 compilaton of 307 supernovae compiled by4 sn z mu dmu.txt (z; µ(z); σ) (SNe) and including supernovae from SNLS,ESSENCE Ωm,ΩΛ,Ωk Survey, HST, and other older sets listed above. H0, w0, wa The Constitution compilation of 397 supernovae 5 Constitution 397 0.015 ! 1.551 by released in 2009 and includes supernovae Ωm,ΩΛ,Ωk sn data const.txt (z; µ(z); σ) (SNe) from the above surveys. H0, w0, wa The Supernoave Cosmology Project (SCP) Union2 557 0.015 ! 1.40 Union 2 compilation of 557 supernovae Ωm,ΩΛ,Ωk sn z mu dmu union2.txt (z; µ(z); σ) 6 (SNe) by including many of the above older sets. H0, w0, wa The Supernovae Cosmology Project (SCP) Union2.1 580 0.015 ! 1.40 Union 2.1 compilation of 580 supernovae Ωm,ΩΛ,Ωk sn z mu dmu union21.txt (z; µ(z); σ) 7 (SNe) by including many of the above older sets. H0, w0, wa 8 Wei low 2010 release by of 109 Ωm,ΩΛ,Ωk (GRB) 50 0.33 ! 1.331 long Gamma-Ray Bursts (GRBs) H0, w0, wa Wei Low.txt (z; µ(z); σ) Wei high with the well-known Amati relation, Ωm,ΩΛ,Ωk 8 (GRB) 59 1.44 ! 8.1 calibrated 59 GRBs as high-redshift . H0, w0, wa Wei High.txt (z; µ(z); σ) 12 measurements of H(z) derived from differential Ages 12 0.0 ! 1.75 ages measurements of the expansion history of the Ωm,ΩΛ,Ωk agesdata plus.txt (z; H(z); σ) 9 (H(z)) universe using LRG galaxy clusters . H0, w0, wa SDSS 0.24 3 direct measurements of H(z) from the Sloan DR6, DR7 3 0.34 Digital Sky Survey (SDSS) Data Releases 6 and 7 Ωm,ΩΛ,Ωk SDSSDR67Hz.txt (z; H(z); σ) 10 (H(z)) 0.43 from LRG galaxy clusters . H0, w0, wa 1 direct measurement of H(z) from the first year BOSS I 1 0.57 release of the Baryon Oscillation Spectroscopic Ωm,ΩΛ,Ωk BOSSIHz.txt (z; H(z); σ) 11 (H(z)) Survey (BOSS) project from the SDSS-III . H0, w0, wa 19 measurements of H(z), 12 from Ages (above) MaStroBC03 19 0.0 ! 1.75 added to the latest from old elliptical galaxies Ωm,ΩΛ,Ωk MaStroBC03.txt (z; H(z); σ) 12 (H(z)) from M. Moresco, et al. H0, w0, wa SDSS 2 measurements of the ratio rs(zd)=DV (z) from Ωm,ΩΛ,Ωk DR7 2 0.20 the Sloan Digital Sky Survey (SDSS) Data H0, w0, wa SDSSDR7BAO.txt (z; rs=DV ; σ) 13 (BAO) 0.35 Release 7 of LRG galaxy clusters . Ωc,Ωb Ωm,ΩΛ,Ωk 6dFGS 1 0.106 1 measurement of the ratio rs(zd)=DV (z) from H0, w0, wa 6dFBAO.txt (z; rs=DV ; σ) 14 (BAO) the 6 degree-Field Galaxy Survey (6dFGS) . Ωc,Ωb 0.44 Ωm,ΩΛ,Ωk WiggleZ 3 0.60 3 measurements of the ratio rs(zd)=DV (z) from H0, w0, wa WiggleZ.txt (z; rs=DV ; σ) 15 (BAO) 0.73 the WiggleZ dark energy survey . Ωc,Ωb 1 measurement of the ratio rs(zd)=DV (z) from BOSS I 1 0.57 the first year release of the Baryon Oscillation Ωm,ΩΛ,Ωk BOSSIBAO.txt (z; rs=DV ; σ) (BAO) Spectroscopic Survey (BOSS) project from the H0, w0, wa 16 SDSS-III . Ωc,Ωb Ωm,ΩΛ,Ωk All 7 7 0.0106 ! 0.73 We compiled all 7 BAO into one list for a H0, w0, wa bao 7.txt (z; rs=DV ; σ) (BAO) quick comparison.
Load more

Recommended publications
  • Pushing the Limits of the Coronagraphic Occulters on Hubble Space Telescope/Space Telescope Imaging Spectrograph
    Pushing the limits of the coronagraphic occulters on Hubble Space Telescope/Space Telescope Imaging Spectrograph John H. Debes Bin Ren Glenn Schneider John H. Debes, Bin Ren, Glenn Schneider, “Pushing the limits of the coronagraphic occulters on Hubble Space Telescope/Space Telescope Imaging Spectrograph,” J. Astron. Telesc. Instrum. Syst. 5(3), 035003 (2019), doi: 10.1117/1.JATIS.5.3.035003. Downloaded From: https://www.spiedigitallibrary.org/journals/Journal-of-Astronomical-Telescopes,-Instruments,-and-Systems on 02 Jul 2019 Terms of Use: https://www.spiedigitallibrary.org/terms-of-use Journal of Astronomical Telescopes, Instruments, and Systems 5(3), 035003 (Jul–Sep 2019) Pushing the limits of the coronagraphic occulters on Hubble Space Telescope/Space Telescope Imaging Spectrograph John H. Debes,a,* Bin Ren,b,c and Glenn Schneiderd aSpace Telescope Science Institute, AURA for ESA, Baltimore, Maryland, United States bJohns Hopkins University, Department of Physics and Astronomy, Baltimore, Maryland, United States cJohns Hopkins University, Department of Applied Mathematics and Statistics, Baltimore, Maryland, United States dUniversity of Arizona, Steward Observatory and the Department of Astronomy, Tucson Arizona, United States Abstract. The Hubble Space Telescope (HST)/Space Telescope Imaging Spectrograph (STIS) contains the only currently operating coronagraph in space that is not trained on the Sun. In an era of extreme-adaptive- optics-fed coronagraphs, and with the possibility of future space-based coronagraphs, we re-evaluate the con- trast performance of the STIS CCD camera. The 50CORON aperture consists of a series of occulting wedges and bars, including the recently commissioned BAR5 occulter. We discuss the latest procedures in obtaining high-contrast imaging of circumstellar disks and faint point sources with STIS.
    [Show full text]
  • Correction: Corrigendum: the Superluminous Transient ASASSN
    LETTERS PUBLISHED: 12 DECEMBER 2016 | VOLUME: 1 | ARTICLE NUMBER: 0002 The superluminous transient ASASSN-15lh as a tidal disruption event from a Kerr black hole G. Leloudas1,​2*, M. Fraser3, N. C. Stone4, S. van Velzen5, P. G. Jonker6,​7, I. Arcavi8,​9, C. Fremling10, J. R. Maund11, S. J. Smartt12, T. Krühler13, J. C. A. Miller-Jones14, P. M. Vreeswijk1, A. Gal-Yam1, P. A. Mazzali15,​16, A. De Cia17, D. A. Howell8,​18, C. Inserra12, F. Patat17, A. de Ugarte Postigo2,​19, O. Yaron1, C. Ashall15, I. Bar1, H. Campbell3,​20, T.-W. Chen13, M. Childress21, N. Elias-Rosa22, J. Harmanen23, G. Hosseinzadeh8,​18, J. Johansson1, T. Kangas23, E. Kankare12, S. Kim24, H. Kuncarayakti25,​26, J. Lyman27, M. R. Magee12, K. Maguire12, D. Malesani2, S. Mattila3,​23,​28, C. V. McCully8,​18, M. Nicholl29, S. Prentice15, C. Romero-Cañizales24,​25, S. Schulze24,​25, K. W. Smith12, J. Sollerman10, M. Sullivan21, B. E. Tucker30,​31, S. Valenti32, J. C. Wheeler33 and D. R. Young12 8 12,13 When a star passes within the tidal radius of a supermassive has a mass >10 M⊙ , a star with the same mass as the Sun black hole, it will be torn apart1. For a star with the mass of the could be disrupted outside the event horizon if the black hole 8 14 Sun (M⊙) and a non-spinning black hole with a mass <10 M⊙, were spinning rapidly . The rapid spin and high black hole the tidal radius lies outside the black hole event horizon2 and mass can explain the high luminosity of this event.
    [Show full text]
  • Report from the Dark Energy Task Force (DETF)
    Fermi National Accelerator Laboratory Fermilab Particle Astrophysics Center P.O.Box 500 - MS209 Batavia, Il l i noi s • 60510 June 6, 2006 Dr. Garth Illingworth Chair, Astronomy and Astrophysics Advisory Committee Dr. Mel Shochet Chair, High Energy Physics Advisory Panel Dear Garth, Dear Mel, I am pleased to transmit to you the report of the Dark Energy Task Force. The report is a comprehensive study of the dark energy issue, perhaps the most compelling of all outstanding problems in physical science. In the Report, we outline the crucial need for a vigorous program to explore dark energy as fully as possible since it challenges our understanding of fundamental physical laws and the nature of the cosmos. We recommend that program elements include 1. Prompt critical evaluation of the benefits, costs, and risks of proposed long-term projects. 2. Commitment to a program combining observational techniques from one or more of these projects that will lead to a dramatic improvement in our understanding of dark energy. (A quantitative measure for that improvement is presented in the report.) 3. Immediately expanded support for long-term projects judged to be the most promising components of the long-term program. 4. Expanded support for ancillary measurements required for the long-term program and for projects that will improve our understanding and reduction of the dominant systematic measurement errors. 5. An immediate start for nearer term projects designed to advance our knowledge of dark energy and to develop the observational and analytical techniques that will be needed for the long-term program. Sincerely yours, on behalf of the Dark Energy Task Force, Edward Kolb Director, Particle Astrophysics Center Fermi National Accelerator Laboratory Professor of Astronomy and Astrophysics The University of Chicago REPORT OF THE DARK ENERGY TASK FORCE Dark energy appears to be the dominant component of the physical Universe, yet there is no persuasive theoretical explanation for its existence or magnitude.
    [Show full text]
  • Detection of Large-Scale X-Ray Bubbles in the Milky Way Halo
    Detection of large-scale X-ray bubbles in the Milky Way halo P. Predehl1†, R. A. Sunyaev2,3†, W. Becker1,4, H. Brunner1, R. Burenin2, A. Bykov5, A. Cherepashchuk6, N. Chugai7, E. Churazov2,3†, V. Doroshenko8, N. Eismont2, M. Freyberg1, M. Gilfanov2,3†, F. Haberl1, I. Khabibullin2,3, R. Krivonos2, C. Maitra1, P. Medvedev2, A. Merloni1†, K. Nandra1†, V. Nazarov2, M. Pavlinsky2, G. Ponti1,9, J. S. Sanders1, M. Sasaki10, S. Sazonov2, A. W. Strong1 & J. Wilms10 1Max-Planck-Institut für Extraterrestrische Physik, Garching, Germany. 2Space Research Institute of the Russian Academy of Sciences, Moscow, Russia. 3Max-Planck-Institut für Astrophysik, Garching, Germany. 4Max-Planck-Institut für Radioastronomie, Bonn, Germany. 5Ioffe Institute, St Petersburg, Russia. 6M. V. Lomonosov Moscow State University, P. K. Sternberg Astronomical Institute, Moscow, Russia. 7Institute of Astronomy, Russian Academy of Sciences, Moscow, Russia. 8Institut für Astronomie und Astrophysik, Tübingen, Germany. 9INAF-Osservatorio Astronomico di Brera, Merate, Italy. 10Dr. Karl-Remeis-Sternwarte Bamberg and ECAP, Universität Erlangen-Nürnberg, Bamberg, Germany. †e-mail: [email protected]; [email protected]; [email protected]; [email protected]; [email protected]; [email protected] The halo of the Milky Way provides a laboratory to study the properties of the shocked hot gas that is predicted by models of galaxy formation. There is observational evidence of energy injection into the halo from past activity in the nucleus of the Milky Way1–4; however, the origin of this energy (star formation or supermassive-black-hole activity) is uncertain, and the causal connection between nuclear structures and large-scale features has not been established unequivocally.
    [Show full text]
  • Perrett RTA.Pdf
    The Astronomical Journal, 140:518–532, 2010 August doi:10.1088/0004-6256/140/2/518 C 2010. The American Astronomical Society. All rights reserved. Printed in the U.S.A. REAL-TIME ANALYSIS AND SELECTION BIASES IN THE SUPERNOVA LEGACY SURVEY∗ K. Perrett1,2, D. Balam3, M. Sullivan4, C. Pritchet5, A. Conley1,6, R. Carlberg1,P.Astier7, C. Balland7,S.Basa8, D. Fouchez9,J.Guy7, D. Hardin7,I.M.Hook3,10, D. A. Howell11,12,R.Pain7, and N. Regnault7 1 Department of Astronomy and Astrophysics, University of Toronto, 50 St. George Street, Toronto, ON, M5S 3H4, Canada; [email protected] 2 Network Information Operations, DRDC Ottawa, 3701 Carling Avenue, Ottawa, ON K1A 0Z4, Canada 3 Dominion Astrophysical Observatory, Herzberg Institute of Astrophysics, 5071 West Saanich Road, Victoria, BC V9E 2E7, Canada 4 Department of Physics (Astrophysics), University of Oxford, DWB, Keble Road, Oxford OX1 3RH, UK; [email protected] 5 Department of Physics & Astronomy, University of Victoria, P.O. Box 3055, Stn CSC, Victoria, BC V8W 3P6, Canada 6 Center for Astrophysics and Space Astronomy, University of Colorado, 593 UCB, Boulder, CO 80309-0593, USA 7 LPNHE, CNRS-IN2P3 and University of Paris VI & VII, 75005 Paris, France 8 Laboratoire d’Astrophysique de Marseille, Poledel’ˆ Etoile´ Site de Chateau-Gombert,ˆ 38, rue Fred´ eric´ Joliot-Curie, 13388 Marseille cedex 13, France 9 CPPM, CNRS-IN2P3 and University Aix Marseille II, Case 907, 13288 Marseille cedex 9, France 10 INAF, Osservatorio Astronomico di Roma, via Frascati 33, 00040 Monteporzio (RM), Italy 11 Las Cumbres Observatory Global Telescope Network, 6740 Cortona Dr., Suite 102, Goleta, CA 93117, USA 12 Department of Physics, University of California, Santa Barbara, Broida Hall, Mail Code 9530, Santa Barbara, CA 93106-9530, USA Received 2010 February 17; accepted 2010 June 4; published 2010 July 1 ABSTRACT The Supernova Legacy Survey (SNLS) has produced a high-quality, homogeneous sample of Type Ia supernovae (SNe Ia) out to redshifts greater than z = 1.
    [Show full text]
  • Publications RENOIR – 24 Sep 2021 Article
    Publications RENOIR { 24 Sep 2021 article 2021 1. The Completed SDSS-IV extended Baryon Oscillation Spectroscopic Survey: one thousand multi-tracer mock catalogues with redshift evolution and systematics for galaxies and quasars of the final data release, C. Zhao et al., Mon. Not. Roy. Astron. Soc 503 (2021) 1149-1173 2. Euclid preparation: XI. Mean redshift determination from galaxy redshift probabilities for cosmic shear tomography, O. Ilbert et al., Euclid Collaboration, Astron. Astrophys. 647 (2021) A117 2020 1. Improving baryon acoustic oscillation measurement with the combination of cosmic voids and galaxies, C. Zhao et al., SDSS Collaboration, Mon. Not. Roy. Astron. Soc 491 (2020) 4554-4572 2. Strong Dependence of Type Ia Supernova Standardization on the Local Specific Star Formation Rate, M. Rigault et al., Nearby Supernova Factory Collaboration, Astron. Astrophys. 644 (2020) A176 3. High-precision Monte-Carlo modelling of galaxy distribution, P. Baratta et al., Astron. Astrophys. 633 (2020) A26 4. Constraints on the growth of structure around cosmic voids in eBOSS DR14, A. J. Hawken et al., J. Cosmol. Astropart. P 2006 (2020) 012 5. SUGAR: An improved empirical model of Type Ia Supernovae based on spectral features, P.-F. L´eget et al., Nearby Supernova Factory Collaboration, Astron. Astrophys. 636 (2020) A46 6. Euclid: Reconstruction of Weak Lensing mass maps for non- Gaussianity studies, S. Pires et al., Euclid Collaboration, Astron. Astrophys. 638 (2020) A141 7. Euclid preparation: VII. Forecast validation for Euclid cosmological probes, A. Blanchard et al., Euclid Collaboration, Astron. Astrophys. 642 (2020) A191 8. Euclid preparation: VI. Verifying the Performance of Cosmic Shear Experiments, P.
    [Show full text]
  • Observations of Comet IRAS-Araki-Alcock (1983D) at La Silla T
    - 12 the visual by 1.3 mag). Like for the other SOor variables we M explain this particular finding by the very high mass loss (M = Bol 5 6.10- M0 yr-') during outburst. The variations in the visual are caused by bolometric flux redistribution in the envelope whilst -10 the bolometric luminosity remains practically constant. The location of R127 in the Hertzsprung-Russell diagram together with the other two known SOor variables of the LMC -B are shown in fig. 8. We note that Walborn classified R127 as an Of or alterna­ tively as a late WN-type star. This indicates that the star is a late Of star evolving right now towards a WN star. Since we have -6 detected an SOor-type outburst of this star we conclude that this transition is not a smooth one but is instead accompanied '.8 '.6 4.0 3.6 by the occasional ejection of dense envelopes. Fig. 8: Location of the newly discovered S Dar variable R 127 in the References Hertzsprung-Russell diagram in comparison with the other two estab­ lished SOor variables of the LMG. Also included in the figure is the Conti, P. S.: 1976, Mem. Soc. Roy. Sei. Liege 9,193. upper envelope of known stellar absolute bolometric magnitudes as Dunean, J. C.: 1922, Publ. Astron. Soc. Pacific 34, 290. derived byHumphreys andDavidson (1979). The approximateposition Hubble, E., Sandage, A.: 1953, Astrophys. J. 118, 353. o( the late WN-type stars is also given. Humphreys, R. M., Davidson, K.: 1979, Astrophys. J. 232,409. Lamers, H.
    [Show full text]
  • World Space Observatory %Uf02d Ultraviolet Remains Very Relevant
    WORLD SPACE OBSERVATORY-ULTRAVIOLET Boris Shustov, Ana Inés Gómez de Castro, Mikhail Sachkov UV observatories aperture pointing mode , Å OAO-2 1968.12 - 1973.01 20 sp is 1000-4250 TD-1A 1972.03 - 1974.05 28 s is 1350-2800+ OAO-3 1972.08 - 1981.02 80 p s 900-3150 ANS 1974.08 - 1977.06 22 p s 1500-3300+ IUE 1978.01 - 1996.09 45 p s 1150-3200 ASTRON 1983.03 - 1989.06 80 p s 1100-3500+ EXOSAT 1983.05 - 1986. 2x30 p is 250+ ROSAT 1990.06 - 1999.02 84 sp i 60- 200+ HST 1990.04 - 240 p isp 1150-10000 EUVE 1992.06 - 2001.01 12 sp is 70- 760 ALEXIS 1993.04 - 2005.04 35 s i 130- 186 MSX 1996.04 - 2003 50 s i 1100-9000+ FUSE 1999.06 - 2007.07 39х35 (4) p s 905-1195 XMM 1999.12 - 30 p is 1700-5500 GALEX 2003.04 - 2013.06 50 sp is 1350-2800 SWIFT 2004.11 - 30 p i 1700-6500 2 ASTROSAT/UVIT UVIT - UltraViolet Imaging Telescopes (on the ISRO Astrosat observatory, launch 2015); Two 40cm telescopes: FUV and NUV, FOV 0.5 degrees, resolution ~1” Next talk by John Hutchings! 3 4 ASTRON (1983 – 1989) ASTRON is an UV space observatory with 80 cm aperture telescope equipped with a scanning spectrometer:(λλ 110-350 nm, λ ~ 2 nm) onboard. Some significant results: detection of OH (H2O) in Halley comet, UV spectroscopy of SN1987a, Pb lines in stellar spectra etc. (Photo of flight model at Lavochkin Museum).5 “Spektr” (Спектр) missions Federal Space Program (2016-2025) includes as major astrophysical projects: Spektr-R (Radioastron) – launched in 2011.
    [Show full text]
  • Euclid: Superluminous Supernovae in the Deep Survey? C
    A&A 609, A83 (2018) Astronomy DOI: 10.1051/0004-6361/201731758 & c ESO 2018 Astrophysics Euclid: Superluminous supernovae in the Deep Survey? C. Inserra1; 2, R. C. Nichol3, D. Scovacricchi3, J. Amiaux4, M. Brescia5, C. Burigana6; 7; 8, E. Cappellaro9, C. S. Carvalho30, S. Cavuoti5; 11; 12, V. Conforti13, J.-C. Cuillandre4; 14; 15, A. da Silva10; 16, A. De Rosa13, M. Della Valle5; 17, J. Dinis10; 16, E. Franceschi13, I. Hook18, P. Hudelot19, K. Jahnke20, T. Kitching21, H. Kurki-Suonio22, I. Lloro23, G. Longo11; 12, E. Maiorano13, M. Maris24, J. D. Rhodes25, R. Scaramella26, S. J. Smartt2, M. Sullivan1, C. Tao27; 28, R. Toledo-Moreo29, I. Tereno16; 30, M. Trifoglio13, and L. Valenziano13 (Affiliations can be found after the references) Received 11 August 2017 / Accepted 3 October 2017 ABSTRACT Context. In the last decade, astronomers have found a new type of supernova called superluminous supernovae (SLSNe) due to their high peak luminosity and long light-curves. These hydrogen-free explosions (SLSNe-I) can be seen to z ∼ 4 and therefore, offer the possibility of probing the distant Universe. Aims. We aim to investigate the possibility of detecting SLSNe-I using ESA’s Euclid satellite, scheduled for launch in 2020. In particular, we study the Euclid Deep Survey (EDS) which will provide a unique combination of area, depth and cadence over the mission. Methods. We estimated the redshift distribution of Euclid SLSNe-I using the latest information on their rates and spectral energy distribution, as well as known Euclid instrument and survey parameters, including the cadence and depth of the EDS.
    [Show full text]
  • Annexe: Summary of Soviet and Russian Space Science Missions
    Contents Introduction by the authors ..................................... ix Acknowledgments ............................................ xi Glossary .................................................. xiii Terminological and translation notes ..............................xv Reference notes .............................................xvii List of tables ............................................... xix List of illustrations ......................................... xxiii List of figures .............................................xxvii 1 Early space science ........................................... 1 Space science by balloon....................................... 3 Scientific flights into the atmosphere: the Akademik series..............14 Scientific test flights with animals ................................20 The idea of a scientific Earth satellite .............................23 Scientific objectives of the first Earth satellites . ....................25 Key people .................................................25 Instead, Prosteishy Sputnik .....................................27 PS2......................................................29 Object D: the first large scientific satellite in orbit....................33 Early space science: what was learned? ............................37 References .................................................39 2 Deepening our understanding ....................................43 Following Sputnik: the MS series ................................43 Cosmos 5 and Starfish: introducing Yuri Galperin
    [Show full text]
  • The World Space Observatory: Ultraviolet Mission: Science Program and Status Report
    PROCEEDINGS OF SPIE SPIEDigitalLibrary.org/conference-proceedings-of-spie The World Space Observatory: ultraviolet mission: science program and status report Sachkov, M., Gómez de Castro, A. I., Shustov, B. M. Sachkov, A. I. Gómez de Castro, B. Shustov, "The World Space Observatory: ultraviolet mission: science program and status report," Proc. SPIE 11444, Space Telescopes and Instrumentation 2020: Ultraviolet to Gamma Ray, 1144473 (13 December 2020); doi: 10.1117/12.2562929 Event: SPIE Astronomical Telescopes + Instrumentation, 2020, Online Only Downloaded From: https://www.spiedigitallibrary.org/conference-proceedings-of-spie on 19 Jan 2021 Terms of Use: https://www.spiedigitallibrary.org/terms-of-use The World Space Observatory - Ultraviolet mission: science program and status report M. Sachkov*a , A.I. Gómez de Castrob, B. Shustova aInstitute of Astronomy of Russian Academy of Sciences, Pyatnitskaya str., 48, Moscow, 119017, Russia; bAEGORA Research Group, Fac. CC. Matematicas, Universidad Complutense, Plaza de Ciencias 3, 28040, Madrid, Spain ABSTRACT A general description of the international space mission "Spectr-UF" (World Space Observatory-Ultraviolet) is given. The project is aimed to create a large space telescope to work in the UV wavelength domain (115 - 310 nm). In the Federal Space Program of Russia for 2016-2025 the launch of the project is scheduled for 2025. We implement several important improvements: updated scientific program of the project; a new design of the Field Camera Unit instrument; corrected orbit; developed a system of collecting applications etc. This paper briefly describes the current status of the mission. Keywords: ultraviolet, spectroscopy, imaging, exoplanet, UV space telescope, WSO-UV 1. INTRODUCTION The Earth's atmosphere blocks observations of celestial objects in the ultraviolet (UV) part of the electromagnetic spectrum.
    [Show full text]
  • The Status of the Hubble Space Telescope
    al insights into the atmospheric struc- ture of hot stars. It is essential, although time consum- ing, to disentangle effects due to binari- ty from effects reflecting the kinematics of the stellar group (11). Especially the lack of recognition of wider binaries with an RV amplitude of the order of 10 kmls might significantly influence the conclu- sions. Hence, repetition of RV observa- tions is necessary and will in turn in- crease our knowledge on binarity in the selected young stellar groups. The spectra will in addition allow a study of stellar rotation in these star groups (12). In many respects, this project forms an extension towards the earliest spec- tral types of the key programmes of Mayor et al. and Gerbaldi et al. (de- scribed in the Messenger 56), even when the primary scientific motivation is somewhat different. In addition to the common interest in radial velocities, the stars in Sco-Cen are also observed by the Hipparcos satellite, providing space motions when combined with the RVs. Using these, we hope to reconstruct the initial minimal volumes in which the star formation occurred which gave rise to the presently expanding Sco-Cen sub- 4180 4200 4220 4240 4260 4280 groups, and to discuss the possibility of wavelength (angstrom) sequential star formation (13). Part of the CASPEC spectrum of NGC 2244-201, a 10th magnitude B 1 V star. The strongest lines are 011 4185, 011 4 190, NII 4242, 011 4254, CII 4267, a complex of 011 lines around First Results 4277A, 011 4283, Slll4285 and 011 4286. Strictly within the frame of the key programme, the first spectra have been obtained on 3 nights in May 1990.
    [Show full text]