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IUCAA Bulletin 2016
Editor : Editorial Assistant : Somak Raychaudhury Manjiri Mahabal ([email protected]) ([email protected]) A quarterly bulletin of the Inter-University Centre for Astronomy and Astrophysics ISSN 0972-7647 (An autonomous institution of the University Grants Commission) Available online at http://ojs.iucaa.ernet.in/ 27th IUCAA Foundation Day Lecture Introduction A Natural History of The 27th IUCAA Foundation Day Knowledge Lecture was delivered by the eminent A naturalist lives today in a world of Indian ecologist, Professor Madhav wounds, but for a connoisseur of Gadgil on December 29, 2015. Over a knowledge, ours is a golden age; the career spanning more than four decades, challenge before us is to deploy the strengths Professor Gadgil has championed the of our age to heal the wounds. Life is an effort towards the preservation of information-based, progressive and ecology in India, which includes cooperative enterprise, evolving organisms establishing the Centre for Ecological capable of handling greater and greater Sciences under the aegis of the Indian quantities, of increasingly more complex Institute of Science, Bengaluru in 1983 information, ever more effectively. Social and serving as the Head of the Western animals have taken this to new heights, with be unhappy in this as well as the nether Ghats Ecology Expert Panel of 2010, humans surpassing them, all thanks to the world. The ruling classes have always tried popularly known as the Gadgil language abilities, and the greatly enhanced to keep the populace ignorant as preached Commission. An alumnus of Harvard capacity to learn, teach, and to elaborate by Laozi, a contemporary of Buddha: The University, he is a recipient of the Padma memes, including mythologies and people are hard to rule when they have too Shri and Padma Bhushan from the scientific knowledge. -
Large-Scale Structure Under Λ-CDM Paradigm
Large-Scale Structure under Λ-CDM Paradigm Timothy Faerber Astrophysical Tests of Physical Theories - May 2020 1 Introduction We live in a universe dominated by matter and energy. On the smallest scale, all matter and energy is composed of \elementary particles", as predicted by the standard model of particle physics, seen in Figure 1. Figure 1: The Standard Model of Particle Physics All of these particles interact or are influenced via one of the four funda- mental forces of nature: the electromagnetic force (responsible for every- day forces, i.e. friction and tension), the nuclear weak force (responsible 1 for beta decay), the nuclear strong force (responsible for binding of neu- trons and electrons to form more atoms), and the gravitational force (responsible for the gravitational attraction between two massive bod- ies) [4]. In this paper we will focus on the gravitational force and the effect that it has on carving out the Large-Scale Structure (LSS) that we see when observing our universe on the scale of superclusters of galaxies (≈ 110 − 130h−1Mpc) [5]. The LSS in our universe is composed of many gravitationally-bound smaller-scale structures such as groups of galax- ies (less than ≈ 30 − 50 giant galaxies, individual galaxies, gas clouds, stars and planets. On scales the size of superclusters, gravity dominates the other three fundamental forces, however without them, small-scale structures could not exist to form the LSS observed. Responsible for holding together every atom in the universe, and thus making it possi- ble for matter to exist as we know it, is the electromagnetic force. -
Probing the Universe at Low Radio Frequencies Using the GMRT
The GMRT : a look at the Past, Present and Future Yashwant Gupta & Govind Swarup National Centre for Radio Astrophysics Pune India URSI GASS Montreal 2017 The GMRT : a look at the Past, Present and Future Yashwant Gupta & Govind Swarup National Centre for Radio Astrophysics Pune India URSI GASS Montreal 2017 Overview of today’s talk . Part I : the GMRT -- a historical perspective . Part II : the GMRT -- current status . Part III : future -- the upgraded GMRT Some history . It is the early 1980s… the VLA has recently become operational . Radio astronomy has shifted from the low frequencies, where it was born, to higher frequencies (cm and higher wavelengths) -- obvious reasons . Note, however, techniques like self-cal have been shown to work . In India, the radio astronomy group at the Tata Institute, under the leadership of Govind Swarup, is looking for the next big challenge… They have already : . Built the Ooty Radio Telescope in the late 1960s – still operational & producing international quality results (in fact, currently being upgraded with new receiver system!) . Built the Ooty Synthesis Radio Telescope (1980s) – short-lived but valuable learnings . Built up considerable experience in low frequencies (metre wavelengths) Birth of the GMRT . Motivation : bridge the gap in radio astronomy facilities at low frequencies and address science problems best studied at metre wavelengths . First concept : 1984 (started with large cylinders); evolved to 34 dishes of 45 metres by 1986 . Project cleared and funding secured by 1987 . Construction started : 1990; first antenna erected : 1992 . First light observations : 1997 – 1998 . Released for world-wide use : 2002 The GMRT : turning it ON Jan 1997 : First fringes with the prototype GMRT correlator Dec 1998 : first light pulsar observation with the GMRT Dedication of the GMRT The Giant Metrewave Radio Telescope was dedicated to the World Scientific Community by the Chairman of TIFR Council, Shri Ratan Tata. -
Revised Classification of the SBS Carbon Star Candidates Including
Astronomy & Astrophysics manuscript no. Carbon˙astroph c ESO 2018 October 8, 2018 Revised classification of the SBS carbon star candidates including the discovery of a new emission line dwarf carbon star ⋆ (Research Note) C. Rossi1, K. S. Gigoyan2, M. G. Avtandilyan3, and S. Sclavi.1 1 Department of Physics, University La Sapienza, Piazza A.Moro 00185, Roma, Italy e-mail: [email protected] 2 V. A. Ambartsumian Byurakan Astrophysical Observatory(BAO)and Isaac Newton Institute of Chile, Armenian Branch, Byurakan 0213, Aragatzotn province, Armenia, e-mail: [email protected] 3 Armenian State Pedagogical Uniiversity After Kh. Abovyan and Isaac Newton Institute of Chile, Armenian Branch, Armenia. e-mail: mar [email protected] Received February 28, 2011 ; accepted ABSTRACT Context. Faint high latitude carbon stars are rare objects commonly thought to be distant, luminous giants. For this reason they are often used to probe the structure of the Galactic halo; however more accurate investigation of photometric and spectroscopic surveys has revealed an increasing percentage of nearby objects with luminosities of main sequence stars. Aims. To clarify the nature of the ten carbon star candidates present in the General Catalog of the Second Byurakan Survey (SBS). Methods. We analyzed new optical spectra and photometry and used astronomical databases available on the web. Results. We verified that two stars are N−type giants already confirmed by other surveys. We found that four candidates are M type stars and confirmed the carbon nature of the remaining four stars; the characteristics of three of them are consistent with an early CH giant type. -
Prime Minister Dr Manmohan Singh Gives Away
ISSN 0409-7467 VOL 59 NO 1 15 JANUARY 2009 Prime Minister Dr Manmohan Singh gives away Shanti Swarup Bhatnagar Prizes for 2007 & 2008, CSIR Diamond Jubilee Technology Award for 2007 and CSIR Award for S&T Innovation for Rural Development for 2007 & 2008 Seen on the dais at the CSIR Award Presentation Function: Prime Minister Dr Manmohan Singh (centre), Minister for Science & Technology and Earth Sciences and Vice President, CSIR, Shri Kapil Sibal (left ) and Director General, CSIR, Prof. Samir K. Brahmachari Prime Minister of India and President, CSIR, Dr Manmohan Singh, gave away Shanti Swarup Bhatnagar Prizes for 2007 & 2008. CSIR Diamond Jubilee Technology Award for 2007 and CSIR Award for S&T Innovation for Rural Development for 2007 & 2008, at a glittering function held on 20 December 2008 in the Dr D.S. Kothari Auditorium, DRDO Bhawan, New Delhi. Attended by a galaxy of S&T personnel, the function was presided over by Shri Kapil Sibal, Minister for Science & Technology and Earth Sciences and Vice President, CSIR. Prof Samir K. Brahmachari, Director General, CSIR, proposed a vote of thanks. We bring in this issue, speeches of Dr Manmohan Singh, Shri Kapil Sibal and Prof. Brahmachari on the occasion along with the citations of the prize-winners. 15 JANUARY 2009 1 CSIR Award Function Speech of Prime Minister Dr Manmohan Singh am very pleased to be here in laboratories.” Iyour midst today to give away the It is this energy and this Shanti Swarup Bhatnagar Prizes for enthusiasm of our scientists that we the years 2007 & 2008. I honour and celebrate each year on congratulate each one of the award such events. -
I–Visibility Correlation Somnath Bharadwaj & Shiv K. Sethi
J. Astrophys. Astr. (2001) 22, 293–307 HI Fluctuations at Large Redshifts: I–Visibility correlation Somnath Bharadwaj1 & Shiv K. Sethi2∗ 1Department of Physics and Meteorology & Center for Theoretical Studies, I.I.T. Kharagpur, 721 302, India email: [email protected] 2Raman Research Institute, C. V. Raman Avenue, Sadashivnagar, Bangalore 560 080, India email: [email protected] Received 2002 March 15; accepted 2002 May 31 Abstract. We investigate the possibility of probing the large scale structure in the universe at large redshifts by studying fluctuations in the redshifted 1420 MHz emission from the neutral hydrogen (HI) at early epochs. The neutral hydrogen content of the universe is known from absorp- < tion studies for z ∼ 4.5. The HI distribution is expected to be inhomoge- neous in the gravitational instability picture and this inhomogeneity leads to anisotropy in the redshifted HI emission. The best hope of detecting this anisotropy is by using a large low-frequency interferometric instru- ment like the Giant Meter-Wave Radio Telescope (GMRT). We calculate the visibility correlation function hVν(U)Vν0 (U)i at two frequencies ν and ν0 of the redshifted HI emission for an interferometric observation. In par- ticular we give numerical results for the two GMRT channels centered around ν = 325 MHz and ν = 610 MHz from density inhomogeneity and peculiar velocity of the HI distribution. The visibility correlation is ' 10−10–10−9 Jy2. We calculate the signal-to-noise for detecting the cor- relation signal in the presence of system noise and show that the GMRT might detect the signal for integration times ' 100 hrs. -
Nissim Kanekar 1 Biographical Details
Nissim Kanekar 1 Biographical details : • Date of Birth : 11th September, 1973 • Nationality : Indian • Institute : National Centre for Radio Astrophysics, TIFR, Pune – 411007, India • Phone : +91 – 20 – 2571 9246 • E-mail : [email protected] 2 Career history: • DST Swarnajayanti Fellowship: 2015 – present, National Centre for Radio Astrophysics, India • Associate Professor: 2012 – present, National Centre for Radio Astrophysics, India • DST Ramanujan Fellowship: 2009 – 2014, National Centre for Radio Astrophysics, India • Reader: 2009 – 2012, National Centre for Radio Astrophysics, India • Max Planck Fellowship : 2007 – 2009, National Radio Astronomy Observatory, USA. • Jansky Fellowship : 2004 – 2008, National Radio Astronomy Observatory, USA. • NOVA Fellowship : 2002 – 2004, Kapteyn Institute, University of Groningen, The Netherlands (NL) • Visiting Fellowship : 2000 – 2001, National Centre for Radio Astrophysics, India 3 Formal education : • Ph.D. (Physics): October 2000, University of Pune. Research carried out at NCRA-TIFR, Pune • M. Sc. (Physics): 1995, University of Pune, India • B. Sc. (Physics): 1993, University of Bombay, India 4 Fellowships and Awards : • Shanti Swarup Bhatnagar Award for the Physical Sciences – 2017, awarded by the Council of Scientific and Industrial Research, India • Hari Om Prerit Vikram Sarabhai Award for Space Sciences – 2015, awarded by Physical Research Laboratory, India • DST Swarnajayanti Fellowship: 2015 – present, National Centre for Radio Astrophysics, India • The Delta Lecturership Award: 2014, awarded by the National Central University, Taiwan • DST Ramanujan Fellowship: 2009 – 2014, National Centre for Radio Astrophysics, India • Vainu Bappu Gold Medal of the Astronomical Society of India: 2008 (shared with Niayesh Afshordi) • Max Planck Fellowship : 2007 – 2009, National Radio Astronomy Observatory, USA. • Distinguished Visitor : 12/2005 – 01/2006, Australia Telescope National Facility, Australia. -
Nova Report 2006-2007
NOVA REPORTNOVA 2006 - 2007 NOVA REPORT 2006-2007 Illustration on the front cover The cover image shows a composite image of the supernova remnant Cassiopeia A (Cas A). This object is the brightest radio source in the sky, and has been created by a supernova explosion about 330 year ago. The star itself had a mass of around 20 times the mass of the sun, but by the time it exploded it must have lost most of the outer layers. The red and green colors in the image are obtained from a million second observation of Cas A with the Chandra X-ray Observatory. The blue image is obtained with the Very Large Array at a wavelength of 21.7 cm. The emission is caused by very high energy electrons swirling around in a magnetic field. The red image is based on the ratio of line emission of Si XIII over Mg XI, which brings out the bi-polar, jet-like, structure. The green image is the Si XIII line emission itself, showing that most X-ray emission comes from a shell of stellar debris. Faintly visible in green in the center is a point-like source, which is presumably the neutron star, created just prior to the supernova explosion. Image credits: Creation/compilation: Jacco Vink. The data were obtained from: NASA Chandra X-ray observatory and Very Large Array (downloaded from Astronomy Digital Image Library http://adil.ncsa.uiuc. edu). Related scientific publications: Hwang, Vink, et al., 2004, Astrophys. J. 615, L117; Helder and Vink, 2008, Astrophys. J. in press. -
Large Telescopes and Why We Need Them Transcript
Large telescopes and why we need them Transcript Date: Wednesday, 9 May 2012 - 1:00PM Location: Museum of London 9 May 2012 Large Telescopes And Why we Need Them Professor Carolin Crawford Astronomy is a comparatively passive science, in that we can’t engage in laboratory experiments to investigate how the Universe works. To study any cosmic object outside of our Solar System, we can only work with the light it emits that happens to fall on Earth. How much we can interpret and understand about the Universe around us depends on how well we can collect and analyse that light. This talk is about the first part of that problem: how we improve the collection of light. The key problem for astronomers is that all stars, nebulae and galaxies are so very far away that they appear both very small, and very faint - some so much so that they can’t be seen without the help of a telescope. Its role is simply to collect more light than the unaided eye can, making astronomical sources appear both bigger and brighter, or even just to make most of them visible in the first place. A new generation of electronic detectors have made observations with the eye redundant. We now have cameras to record the images directly, or once it has been split into its constituent wavelengths by spectrographs. Even though there are a whole host of ingenious and complex instruments that enable us to record and analyse the light, they are still only able to work with the light they receive in the first place. -
Carbon Stars T. Lloyd Evans
J. Astrophys. Astr. (2010) 31, 177–211 Carbon Stars T. Lloyd Evans SUPA, School of Physics and Astronomy, University of St. Andrews, North Haugh, St. Andrews, Fife KY16 9SS, UK. e-mail: [email protected] Received 2010 July 19; accepted 2010 October 18 Abstract. In this paper, the present state of knowledge of the carbon stars is discussed. Particular attention is given to issues of classification, evolution, variability, populations in our own and other galaxies, and circumstellar material. Key words. Stars: carbon—stars: evolution—stars: circumstellar matter —galaxies: magellanic clouds. 1. Introduction Carbon stars have been reviewed on several previous occasions, most recently by Wallerstein & Knapp (1998). A conference devoted to this topic was held in 1996 (Wing 2000) and two meetings on AGB stars (Le Bertre et al. 1999; Kerschbaum et al. 2007) also contain much on carbon stars. This review emphasizes develop- ments since 1997, while paying particular attention to connections with earlier work and to some of the important sources of concepts. Recent and ongoing develop- ments include surveys for carbon stars in more of the galaxies of the local group and detailed spectroscopy and infrared photometry for many of them, as well as general surveys such as 2MASS, AKARI and the Sirius near infrared survey of the Magel- lanic Clouds and several dwarf galaxies, the Spitzer-SAGE mid-infrared survey of the Magellanic Clouds and the current Herschel infrared satellite project. Detailed studies of relatively bright galactic examples continue to be made by high-resolution spectroscopy, concentrating on abundance determinations using the red spectral region, and infrared and radio observations which give information on the history of mass loss. -
Barium & Related Stars and Their White-Dwarf Companions II. Main
Astronomy & Astrophysics manuscript no. dBa_orbits c ESO 2019 April 9, 2019 Barium & related stars and their white-dwarf companions ?, ?? II. Main-sequence and subgiant stars A. Escorza1; 2, D. Karinkuzhi2; 3, A. Jorissen2, L. Siess2, H. Van Winckel1, D. Pourbaix2, C. Johnston1, B. Miszalski4; 5, G-M. Oomen1; 6, M. Abdul-Masih1, H.M.J. Boffin7, P. North8, R. Manick1; 4, S. Shetye2; 1, and J. Mikołajewska9 1 Institute of Astronomy, KU Leuven, Celestijnenlaan 200D, B-3001 Leuven, Belgium e-mail: [email protected] 2 Institut d’Astronomie et d’Astrophysique, Université Libre de Bruxelles, Boulevard du Triomphe, B-1050 Bruxelles, Belgium 3 Department of physics, Jnana Bharathi Campus, Bangalore University, Bangalore 560056, India 4 South African Astronomical Observatory, PO Box 9, Observatory 7935, South Africa 5 Southern African Large Telescope Foundation, PO Box 9, Observatory 7935, South Africa 6 Department of Astrophysics/IMAPP, Radboud University, P.O. Box 9010, 6500 GL Nijmegen, The Netherlands 7 ESO, Karl-Schwarzschild-str. 2, 85748 Garching bei München, Germany 8 Institut de Physique, Laboratoire d’astrophysique, École Polytechnique Fédérale de Lausanne (EPFL), Observatoire, 1290 Versoix, Switzerland 9 N. Copernicus Astronomical Center, Polish Academy of Sciences, Bartycka 18, 00-716 Warsaw, Poland Accepted ABSTRACT Barium (Ba) dwarfs and CH subgiants are the less-evolved analogues of Ba and CH giants. They are F- to G-type main-sequence stars polluted with heavy elements by a binary companion when the latter was on the Asymptotic Giant Branch (AGB). This companion is now a white dwarf that in most cases cannot be directly detected. We present a large systematic study of 60 objects classified as Ba dwarfs or CH subgiants. -
Calibration, Foreground Subtraction, and Signal
From Theoretical Promise to Observational Reality: Calibration, Foreground Subtraction, and Signal Extraction in Hydrogen Cosmology by Adrian Chi-Yan Liu A.B., Princeton University (2006) Submitted to the Department of Physics in partial fulfillment of the requirements for the degree of Doctor of Philosophy at the MASSACHUSETTS INSTITUTE OF TECHNOLOGY June 2012 c Massachusetts Institute of Technology 2012. All rights reserved. Author.............................................................. Department of Physics May 25, 2012 Certified by. Max Erik Tegmark Professor of Physics Thesis Supervisor Accepted by . Krishna Rajagopal Professor of Physics Associate Department Head for Education 2 From Theoretical Promise to Observational Reality: Calibration, Foreground Subtraction, and Signal Extraction in Hydrogen Cosmology by Adrian Chi-Yan Liu Submitted to the Department of Physics on May 25, 2012, in partial fulfillment of the requirements for the degree of Doctor of Philosophy Abstract By using the hyperfine 21 cm transition to map out the distribution of neutral hy- drogen at high redshifts, hydrogen cosmology has the potential to place exquisite constraints on fundamental cosmological parameters, as well as to provide direct ob- servations of our Universe prior to the formation of the first luminous objects. How- ever, this theoretical promise has yet to become observational reality. Chief amongst the observational obstacles are a need for extremely well-calibrated instruments and methods for dealing with foreground contaminants such as Galactic synchrotron ra- diation. In this thesis we explore a number of these challenges by proposing and testing a variety of techniques for calibration, foreground subtraction, and signal extraction in hydrogen cosmology. For tomographic hydrogen cosmology experiments, we explore a calibration algorithm known as redundant baseline calibration, extending treatments found in the existing literature to include rigorous calculations of uncertainties and extensions to not-quite-redundant baselines.