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PRECISE PHOTOMETRIC TRANSIT FOLLOW-UP OBSERVATIONS of FIVE CLOSE-IN EXOPLANETS : UPDATE on THEIR PHYSICAL PROPERTIES Aritra Chakrabarty†1, 2 and Sujan Sengupta‡1
Draft version May 28, 2019 Typeset using LATEX default style in AASTeX62 PRECISE PHOTOMETRIC TRANSIT FOLLOW-UP OBSERVATIONS OF FIVE CLOSE-IN EXOPLANETS : UPDATE ON THEIR PHYSICAL PROPERTIES Aritra Chakrabartyy1, 2 and Sujan Senguptaz1 1Indian Institute of Astrophysics, Koramangala 2nd Block, Bangalore 560034, India 2University of Calcutta, Salt Lake City, JD-2, Kolkata 750098, India (Accepted for publication in the Astronomical Journal) ABSTRACT We report the results of the high precision photometric follow-up observations of five transiting hot jupiters - WASP-33b, WASP-50b, WASP-12b, HATS-18b and HAT-P-36b. The observations are made from the 2m Himalayan Chandra Telescope at Indian Astronomical Observatory, Hanle and the 1.3m J. C. Bhattacharyya Telescope at Vainu Bappu Observatory, Kavalur. This exercise is a part of the capability testing of the two telescopes and their back-end instruments. Leveraging the large aperture of both the telescopes used, the images taken during several nights were used to produce the transit light curves with high photometric S/N (> 200) by performing differential photometry. In order to reduce the fluctuations in the transit light curves due to various sources such as stellar activity, varying sky transparency etc. we preprocessed them using wavelet denoising and applied Gaussian process correlated noise modeling technique while modeling the transit light curves. To demonstrate the efficiency of the wavelet denoising process we have also included the results without the denoising process. A state-of-the-art algorithm used for modeling the transit light curves provided the physical parameters of the planets with more precise values than reported earlier. -
Indian Institute of Astrophysics
Indian Institute of Astrophysics The Indian Institute of Astrophysics (IIA), an autonomous research institute funded by the Department of Science & Technology, is devoted to research in Astronomy & Astrophysics, and the Related Physics and Instrumentation. IIA has a rich history of over two centuries and has to its credit some important discoveries such as those of the Evershed effect, atmosphere on Jupiter's satellite Ganymede, the rings around Uranus and the asteroid Ramanujan. Research Programmes Research fields in Astronomy & Astrophysics at IIA range from the studies of the nearby sun and solar system objects to the distant galaxies, quasars and gamma-ray burst sources. Sun and the Solar System - Solar activity - sunspots, prominences; Solar Chromosphere and Corona; Comets; Solar Terrestrial relationships Stellar Physics - Formation and Evolution of Stars; Comet Machholz Planetary Nebulae; Stellar Atmospheres; Star observed from VBO Clusters; Stellar Variability; Novae; Supernovae; Brown Dwarfs, Pulsars Solar Corona Extragalactic Astronomy - Star formation in galaxies; Activity in Galaxies; Groups and Clusters of Galaxies; Gamma-ray burst events Theoretical Astrophysics and Related Physics - Magnetohydrodynamic and Radiative Processes in Astrophysical Objects; Structure of Neutron Stars; Blackhole Physics; Structure and Dynamics of Galaxies and Star Clusters; General Theory of Relativity; Cosmology; Astroparticle Physics; Atomic and Molecular Physics NGC 925 observed with the 2m HCT Instrumentation - UV Imaging Telescope for the Indian Astronomy Satellite (ASTROSAT); back-end instruments for the various observing facilities. Facilities The Institute's research activities are supported by excellent facilities at its headquarters in Bangalore and its field stations at Kodaikanal, Kavalur, Gauribidanur, Hosakote and Hanle. The Solar Observatory: located at Kodaikanal consists of a Tower Tunnel Telescope, Spectroheliographs and Ionosondes. -
Variable Star Section Circular
British Astronomical Association Variable Star Section Circular No 82, December 1994 CONTENTS A New Director 1 Credit for Observations 1 Submission of 1994 Observations 1 Chart Problems 1 Recent Novae Named 1 Z Ursae Minoris - A New R CrB Star? 2 The February 1995 Eclipse of 0¼ Geminorum 2 Computerisation News - Dave McAdam 3 'Stella Haitland, or Love and the Stars' - Philip Hurst 4 The 1994 Outburst of UZ Bootis - Gary Poyner 5 Observations of Betelgeuse by the SPA-VSS - Tony Markham 6 The AAVSO and the Contribution of Amateurs to VS Research Suspected Variables - Colin Henshaw 8 From the Literature 9 Eclipsing Binary Predictions 11 Summaries of IBVS's Nos 4040 to 4092 14 The BAA Instruments and Imaging Section Newsletter 16 Light-curves (TZ Per, R CrB, SV Sge, SU Tau, AC Her) - Dave McAdam 17 ISSN 0267-9272 Office: Burlington House, Piccadilly, London, W1V 9AG Section Officers Director Tristram Brelstaff, 3 Malvern Court, Addington Road, READING, Berks, RG1 5PL Tel: 0734-268981 Section Melvyn D Taylor, 17 Cross Lane, WAKEFIELD, Secretary West Yorks, WF2 8DA Tel: 0924-374651 Chart John Toone, Hillside View, 17 Ashdale Road, Cressage, Secretary SHREWSBURY, SY5 6DT Tel: 0952-510794 Computer Dave McAdam, 33 Wrekin View, Madeley, TELFORD, Secretary Shropshire, TF7 5HZ Tel: 0952-432048 E-mail: COMPUSERV 73671,3205 Nova/Supernova Guy M Hurst, 16 Westminster Close, Kempshott Rise, Secretary BASINGSTOKE, Hants, RG22 4PP Tel & Fax: 0256-471074 E-mail: [email protected] [email protected] Pro-Am Liaison Roger D Pickard, 28 Appletons, HADLOW, Kent TN11 0DT Committee Tel: 0732-850663 Secretary E-mail: [email protected] KENVAD::RDP Eclipsing Binary See Director Secretary Circulars Editor See Director Telephone Alert Numbers Nova and First phone Nova/Supernova Secretary. -
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). -
Astrometry and Optics During the Past 2000 Years
1 Astrometry and optics during the past 2000 years Erik Høg Niels Bohr Institute, Copenhagen, Denmark 2011.05.03: Collection of reports from November 2008 ABSTRACT: The satellite missions Hipparcos and Gaia by the European Space Agency will together bring a decrease of astrometric errors by a factor 10000, four orders of magnitude, more than was achieved during the preceding 500 years. This modern development of astrometry was at first obtained by photoelectric astrometry. An experiment with this technique in 1925 led to the Hipparcos satellite mission in the years 1989-93 as described in the following reports Nos. 1 and 10. The report No. 11 is about the subsequent period of space astrometry with CCDs in a scanning satellite. This period began in 1992 with my proposal of a mission called Roemer, which led to the Gaia mission due for launch in 2013. My contributions to the history of astrometry and optics are based on 50 years of work in the field of astrometry but the reports cover spans of time within the past 2000 years, e.g., 400 years of astrometry, 650 years of optics, and the “miraculous” approval of the Hipparcos satellite mission during a few months of 1980. 2011.05.03: Collection of reports from November 2008. The following contains overview with summary and link to the reports Nos. 1-9 from 2008 and Nos. 10-13 from 2011. The reports are collected in two big file, see details on p.8. CONTENTS of Nos. 1-9 from 2008 No. Title Overview with links to all reports 2 1 Bengt Strömgren and modern astrometry: 5 Development of photoelectric astrometry including the Hipparcos mission 1A Bengt Strömgren and modern astrometry .. -
Indian Institute of Astrophysics Bangalore 560034
Indian Institute of Astrophysics Bangalore 560034 The Indian Institute of Astrophysics (IIA) traces its origin to relativity, cosmology, astroparticle physics, atomic and a small private observatory set up during 1786 at Madras molecular physics. (Chennai), which led to the establishment of the Solar Observatory in 1899 at Kodaikanal. In 1971, the Facilities: Kodaikanal Observatory was made into an autonomous institution under the Department of Science & Technology, Kodaikanal Observatory: This Observatory has been the Government of India. With a rich history of over 200 years, principal center of activity in observational solar physics, IIA is a premier institute in the country devoted to basic for over a century. At present, the main facility is the solar research, instrumentation and training in astronomy, tunnel telescope fitted with a spectrograph, which is in astrophysics and related physical sciences. regular use since 1962; a spectro-polarimeter has also been added. This observatory has a unique collection of the Sun’s photographic images archived over the last hundred years. These images are now being digitized to study the finer details of the Sun, Sun-weather pattern etc. Daily observations of the solar photosphere and chromosphere are being obtained as a part of the synoptic study. It was in this Observatory, John Evershed discovered the radial motion in sunspots, now known as the Evershed effect, in 1909. The Indian Institute of Astrophysics, Bangalore. Research Programmes: Sun and the Solar System - Solar activity, sunspots, prominences, solar chromosphere, comets, asteroids, eclipse observations, radio observations of the solar corona. Stellar Physics - Formation and evolution of stars, chemical abundance of elements, planetary nebulae, planetary rings, The solar tunnel telescope at the Kodaikanal observatory. -
List of Bright Nebulae Primary I.D. Alternate I.D. Nickname
List of Bright Nebulae Alternate Primary I.D. Nickname I.D. NGC 281 IC 1590 Pac Man Neb LBN 619 Sh 2-183 IC 59, IC 63 Sh2-285 Gamma Cas Nebula Sh 2-185 NGC 896 LBN 645 IC 1795, IC 1805 Melotte 15 Heart Nebula IC 848 Soul Nebula/Baby Nebula vdB14 BD+59 660 NGC 1333 Embryo Neb vdB15 BD+58 607 GK-N1901 MCG+7-8-22 Nova Persei 1901 DG 19 IC 348 LBN 758 vdB 20 Electra Neb. vdB21 BD+23 516 Maia Nebula vdB22 BD+23 522 Merope Neb. vdB23 BD+23 541 Alcyone Neb. IC 353 NGC 1499 California Nebula NGC 1491 Fossil Footprint Neb IC 360 LBN 786 NGC 1554-55 Hind’s Nebula -Struve’s Lost Nebula LBN 896 Sh 2-210 NGC 1579 Northern Trifid Nebula NGC 1624 G156.2+05.7 G160.9+02.6 IC 2118 Witch Head Nebula LBN 991 LBN 945 IC 405 Caldwell 31 Flaming Star Nebula NGC 1931 LBN 1001 NGC 1952 M 1 Crab Nebula Sh 2-264 Lambda Orionis N NGC 1973, 1975, Running Man Nebula 1977 NGC 1976, 1982 M 42, M 43 Orion Nebula NGC 1990 Epsilon Orionis Neb NGC 1999 Rubber Stamp Neb NGC 2070 Caldwell 103 Tarantula Nebula Sh2-240 Simeis 147 IC 425 IC 434 Horsehead Nebula (surrounds dark nebula) Sh 2-218 LBN 962 NGC 2023-24 Flame Nebula LBN 1010 NGC 2068, 2071 M 78 SH 2 276 Barnard’s Loop NGC 2149 NGC 2174 Monkey Head Nebula IC 2162 Ced 72 IC 443 LBN 844 Jellyfish Nebula Sh2-249 IC 2169 Ced 78 NGC Caldwell 49 Rosette Nebula 2237,38,39,2246 LBN 943 Sh 2-280 SNR205.6- G205.5+00.5 Monoceros Nebula 00.1 NGC 2261 Caldwell 46 Hubble’s Var. -
Thesis, Anton Pannekoek Institute, Universiteit Van Amsterdam
UvA-DARE (Digital Academic Repository) The peculiar climates of ultra-hot Jupiters Arcangeli, J. Publication date 2020 Document Version Final published version License Other Link to publication Citation for published version (APA): Arcangeli, J. (2020). The peculiar climates of ultra-hot Jupiters. General rights It is not permitted to download or to forward/distribute the text or part of it without the consent of the author(s) and/or copyright holder(s), other than for strictly personal, individual use, unless the work is under an open content license (like Creative Commons). Disclaimer/Complaints regulations If you believe that digital publication of certain material infringes any of your rights or (privacy) interests, please let the Library know, stating your reasons. In case of a legitimate complaint, the Library will make the material inaccessible and/or remove it from the website. Please Ask the Library: https://uba.uva.nl/en/contact, or a letter to: Library of the University of Amsterdam, Secretariat, Singel 425, 1012 WP Amsterdam, The Netherlands. You will be contacted as soon as possible. UvA-DARE is a service provided by the library of the University of Amsterdam (https://dare.uva.nl) Download date:09 Oct 2021 Jacob Arcangeli of Ultra-hot Jupiters The peculiar climates The peculiar climates of Ultra-hot Jupiters Jacob Arcangeli The peculiar climates of Ultra-hot Jupiters Jacob Arcangeli © 2020, Jacob Arcangeli Contact: [email protected] The peculiar climates of Ultra-hot Jupiters Thesis, Anton Pannekoek Institute, Universiteit van Amsterdam Cover by Imogen Arcangeli ([email protected]) Printed by Amsterdam University Press ANTON PANNEKOEK INSTITUTE The research included in this thesis was carried out at the Anton Pannekoek Institute for Astronomy (API) of the University of Amsterdam. -
Arxiv:1505.04244V1 [Astro-Ph.IM] 16 May 2015 .Srinivasulu G
Bull. Astr. Soc. India (2014) 42, 1–19 A new three-band, two beam astronomical photo-polarimeter 1 2 1 3 G. Srinivasulu ∗, A. V. Raveendran , S. Muneer †, M. V. Mekkaden , N. Jayavel4, M. R. Somashekar1, K. Sagayanathan1, S. Ramamoorthy1, 5 6 M. J. Rosario and K. Jayakumar ‡ 1Indian Institute of Astrophysics, Bangalore 560034, India 2399, "Shravanam", 2nd Block, 9th Phase, J P Nagar, Bangalore 560108, India 3No 82, 17E Main, 6th Block, Koramangala, Bangalore 560095, India 4No 22, Bandappa lane, New Byappanahalli, Bangalore 560038, India 5210, 4th Main, Lakshmi Nagar Extn, Porur, Chennai 600116, India 624, Postal Nagar, Ampuram, Vellore-632009, India Received 2014 July 23; revised ; accepted Abstract. We designed and built a new astronomical photo-polarimeter that can meas- ure linear polarization simultaneously in three spectral bands. It has a Calcite beam- displacement prism as the analyzer. The ordinary and extra-ordinary emerging beams in each spectral bands are quasi-simultaneously detected by the same photomultiplier by using a high speed rotating chopper. A rotating superachromatic Pancharatnam halfwave plate is used to modulate the light incident on the analyzer. The spectral bands are isolated using appropriate dichroic and glass filters. We show that the reduction of 50% in the efficiency of the polarimeter because of the fact that the intensities of the two beams are measured alternately is partly com- pensated by the reduced time to be spent on the observation of the sky background. The use of a beam-displacement prism as the analyzer completely removes the polar- ization of backgroundskylight, which is a major source of error during moonlit nights, especially, in the case of faint stars. -
Multi-Band Observations of Gamma Ray Bursts
J. Astrophys. Astr. (2002) 23, 123–127 Multi-band Observations of Gamma Ray Bursts S. G. Bhargavi Indian Institute of Astrophysics, Bangalore 560 034, India email: [email protected] Abstract. This talk focuses on the various aspects we learnt from multi- band observations of GRBs both, before and during the afterglow era. A statistical analysis to estimate the probable redshifts of host galaxies using the luminosity function of GRBs compatible with both the afterglow redshift data as well as the overall population of GRBs is discussed. We then address the question whether the observed fields of GRBs with precise localizations from third Inter-Planetary Network (IPN3) contain suitable candidates for their host galaxies. Key words. Gamma rays: bursts—CCD: observations—Methods: statistical. 1. Studies before the afterglow era In 1994–95 we undertook a program to carry out an optical survey of a few GRB fields chosen from the IPN3 catalog (Hurley 1995, private communication; Laros et al. 1998; Hurley et al. 2000). Deep CCD imaging of these fields was carried out at the 2.34 m and 1.02 m telescopes of Vainu Bappu Observatory (VBO), Kavalur until 1998. It was an attempt to identify the transient/quiescent counterparts of GRBs on the basis of photometric studies. For details on observations and photometric data analysis see Bhargavi (2001). In similar investigations the observers either looked for peculiar objects (Vrba et al. 1995) or an over-abundance of certain class of objects (Larson 1997) in their deep imaging surveys of IPN GRBs. None of our efforts led to an identification of a GRB counterpart. -
1 Introduction 2 Vainu Bappu Observatory, Kavalur, Indian Institute
GROUND-BASED OPTICAL ASTRONOMY IN INDIA M.Parthasarathy, Indian Institute of Astrophysics, Bangalore - 560034 India Abstract There is considerable progress in the ground based optical astronomy in India during the last 25 years. During the period 1965 to 1995 four one meter class telescopes and one 2.3m telescope have corne into operation. The number of users of these facilities has increased considerably. The existing optical telescpes in India are heavily over-subscribed and are not large enough for observing fainter stars and faint and distant galaxies . There is an urgent need to set up at good sites in India 4m class new technology telescopes and a few 1m and 2m class telescopes equipped with upto date auxiliary instruments. 1 Introduction During the last 30 years, a number of telescopes have become available in India for astronomical observations over different regions of the electromagnetic spectrum ranging from Gamma-rays, X-rays, optical, infrared and radio wavelength regions. In this paper the existing facilities for ground-based optical astronomy in India are described. The research work in optical astronomy in India and future plans to set up new 2m to 4m class telescopes are also described. There are five major existing optical telescopes in India: (i) a 1m Carl-Zeiss telescope at Naini Tal, (ii) a 1.2m Baker reflector at Rangapur near Hyderbad, (iii) a 1m Carl-Zeiss telescope and a 2.3m Vainu Bappu Telescope (VBT) at Kava1ur, (iv) a 1.2m infrared telescope at Gurusikhar near Mount Abu. There are also three main solar observatories in India at Kodaikanal, Udaipur and N aini Tal. -
Abstracts of Extreme Solar Systems 4 (Reykjavik, Iceland)
Abstracts of Extreme Solar Systems 4 (Reykjavik, Iceland) American Astronomical Society August, 2019 100 — New Discoveries scope (JWST), as well as other large ground-based and space-based telescopes coming online in the next 100.01 — Review of TESS’s First Year Survey and two decades. Future Plans The status of the TESS mission as it completes its first year of survey operations in July 2019 will bere- George Ricker1 viewed. The opportunities enabled by TESS’s unique 1 Kavli Institute, MIT (Cambridge, Massachusetts, United States) lunar-resonant orbit for an extended mission lasting more than a decade will also be presented. Successfully launched in April 2018, NASA’s Tran- siting Exoplanet Survey Satellite (TESS) is well on its way to discovering thousands of exoplanets in orbit 100.02 — The Gemini Planet Imager Exoplanet Sur- around the brightest stars in the sky. During its ini- vey: Giant Planet and Brown Dwarf Demographics tial two-year survey mission, TESS will monitor more from 10-100 AU than 200,000 bright stars in the solar neighborhood at Eric Nielsen1; Robert De Rosa1; Bruce Macintosh1; a two minute cadence for drops in brightness caused Jason Wang2; Jean-Baptiste Ruffio1; Eugene Chiang3; by planetary transits. This first-ever spaceborne all- Mark Marley4; Didier Saumon5; Dmitry Savransky6; sky transit survey is identifying planets ranging in Daniel Fabrycky7; Quinn Konopacky8; Jennifer size from Earth-sized to gas giants, orbiting a wide Patience9; Vanessa Bailey10 variety of host stars, from cool M dwarfs to hot O/B 1 KIPAC, Stanford University (Stanford, California, United States) giants. 2 Jet Propulsion Laboratory, California Institute of Technology TESS stars are typically 30–100 times brighter than (Pasadena, California, United States) those surveyed by the Kepler satellite; thus, TESS 3 Astronomy, California Institute of Technology (Pasadena, Califor- planets are proving far easier to characterize with nia, United States) follow-up observations than those from prior mis- 4 Astronomy, U.C.