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  • Host galaxies of ultrastrong Mg II absorbers at z ∼ 0.5 
    Guha, Labanya Kumar; Srianand, Raghunathan; Dutta, Rajeshwari; Joshi, Ravi; Noterdaeme, Pasquier; Petitjean, Patrick (Oxford University Press on behalf of Royal Astronomical Society, 2022-07)
    From a sample of 109 candidate ultrastrong Mg II (USMg II; having rest equivalent width of Mg II, W2796 > 3.0 Å) systems at z = 0.4–0.6, we confirm 27 and identify host galaxies of 20 systems based on associated nebular ...
  • Host galaxy magnitude of OJ 287 from its colours at minimum light 
    Valtonen, Mauri J; Dey, Lankeswar; Zola, S; Ciprini, S; Kidger, M; Pursimo, T; Gopakumar, A; Matsumoto, K; Sadakane, K; Caton, D. B; Nilsson, K; Komossa, S; Bagaglia, M; Baransky, A; Boumis, P; Boyd, D; Castro-Tirado, A. J; Debski, B; Drozdz, M; Perez, A. Escartin; Fiorucci, M; Garcia, F; Gazeas, K; Ghosh, S; Godunova, V; Gomez, J. L; Gredel, R; Grupe, D; Haislip, J. B; Henning, T; Hurst, G; Janík, J; Kouprianov, V. V; Lehto, H; Liakos, A; Mathur, S; Mugrauer, M; Nogues, R. Naves; Nucciarelli, G; Ogloza, W; Ojha, D. K; Pajdosz-Śmierciak, U; Pascolini, S; Poyner, G; Reichart, D. E; Rizzi, N; Roncella, F; Sahu, D. K; Sillanpää, A; Simon, A; Siwak, M; Alfaro, F. C. Soldán; Sonbas, E; Tosti, G; Vasylenko, V; Webb, J. R; Zielinski, P (Oxford University Press on behalf of Royal Astronomical Society, 2022-08)
    OJ 287 is a BL Lacertae type quasar in which the active galactic nucleus (AGN) outshines the host galaxy by an order of magnitude. The only exception to this may be at minimum light when the AGN activity is so low that ...
  • Host star metallicity of directly imaged wide-orbit planets: implications for planet formation 
    Swastik, C; Banyal, R. K; Narang, Mayank; Manoj, P; Sivarani, T; Reddy, B. E; Rajaguru, S. P (IOP Publishing, 2021-03-01)
    Directly imaged planets (DIPs) are self-luminous companions of pre-main-sequence and young main-sequence stars. They reside in wider orbits (~tens to thousands of astronomical units) and generally are more massive compared ...
  • Hot and cold spot counts as probes of non-gaussianity in the cosmic microwave background 
    Pravabati, C; Park, C; Yogendran, K. P; van de Weygaert, R (IOP Publishing, 2012-08-20)
    We introduce the numbers of hot and cold spots, n/subh/ and n/subc/, of excursion sets of the cosmic microwave background (CMB) temperature anisotropy maps as statistical observables that can discriminate different ...
  • A hot companion to a blue straggler in NGC 188 as revealed by the ultra-violet imaging telescope (UVIT) on ASTROSAT 
    Subramaniam, A; Sindhu, N; Tandon, S. N; Kameswara Rao, N; Postma, J; Cote, Patrick; Hutchings, J. B; Ghosh, S. K; George, K; Girish, V (IOP Publishing, 2016-12-20)
    We present early results from the Ultra-Violet Imaging Telescope (UVIT) on board the ASTROSAT observatory. We report the discovery of a hot companion associated with one of the blue straggler stars (BSSs) in the old open ...
  • Hot post-AGB stars 
    Parthasarathy, M; Gauba, G; Fujii, T; Nakada, Y (Kluwer Academic Publishers, 2001-08)
    From the study of IRAS sources with far-IR colors similar to planetary nebulae (PNe), several proto-planetary nebulae with hot (OB) post-AGB central stars have been detected. These stars form an evolutionary link between ...
  • The hot R Coronae Borealis star DY Centauri: Nebular and photospheric lines 
    Kameswara Rao, N; Giridhar, S; Lambert, D. L (The European Southern Observatory, 1993-12)
    High resolution spectra in the red region of the hot R CrB star DY Cen show the following characteristics: a strong absorption line spectrum dominated by lines of C II, N II, and Ne I inverse P-Cygni type profiles of some ...
  • The hot γ Doradus and Maia stars 
    Balona, L. A; Engelbrecht, C. A; Joshi, Y. C; Joshi, S; Sharma, K; Semenko, E; Pandey, G; Chakradhari, N. K; Mkrtichian, D; Hema, B. P; Nemec, J. M (Oxford University Press on behalf of the Royal Astronomical Society, 2016-09)
    The hot γ Doradus stars have multiple low frequencies characteristic of γ Dor or SPB variables, but are located between the red edge of the SPB and the blue edge of the γ Dor instability strips where all low-frequency ...
  • How are the observed frequencies related to solar structure? 
    Christensen-Dalsgaard, J (Astronomical Society of India, 1996)
  • How black is a black hole? 
    Kapoor, R. C (Bennett. Coleman & Co., Ltd., 1977-05)
  • How bright are extra-solar planets? 
    Das, S. R (Astronomical Society of India, 1996)
  • How CMB and large-scale structure constrain chameleon interacting dark energy 
    Boriero, Daniel; Das, Subinoy; Wong, Yvonne Y. Y (IOP Publishing, 2015-06)
    We explore a chameleon type of interacting dark matter-dark energy scenario in which a scalar field adiabatically traces the minimum of an eff ective potential sourced by the dark matter density. We discuss extensively ...
  • How does the presence of bar affects the fueling of supermassive black holes? An IllustrisTNG100 perspective 
    Kataria, Sandeep Kumar; Vivek, M (Oxford University Press on behalf of Royal Astronomical Society, 2024-01)
    We conducted a statistical study of black hole masses of barred and unbarred galaxies in the IllustrisTNG100 cosmological magnetohydrodynamical simulations. This work aims to understand the role of the bars in the growth ...
  • How impossible is topology change? 
    Borde, A (Astronomical Society of India, 1997)
    It is often stated that topology change is impossible in classical general relativity. In particular, it appears to be widely believed that the pleasure of topology change comes at a fixed price: topology – changing space ...
  • How late can the dark matter form in our universe? 
    Sarkar, A; Das, Subinoy; Sethi, Shiv K (IOP Publishing, 2015-03)
    We put constraints on the epoch of dark matter formation for a class of non-WIMP (Weakly Interacting Massive Particle) dark matter candidates. These models allow a fraction of Cold Dark Matter (CDM) to be formed between ...
  • How Normal are the Peculiar A-Stars 
    Babu, G. S. D; Shylaja, B. S (Astronomical Society of the Pacific, 1993-02)
  • How Thick are the Saturn's Rings? 
    Chakrabarti, S. K; Bhattacharyya, A (Astronomical Society of India, 2002-09)
    It has been long thought that the rings of saturn are probably not thicker than a few hundreds of meters. By actually following the motion of particles inside the decaying bending waves of the Saturn's rings and matching the ...
  • How well do we know our Sun? 
    Chitre, S. M (Indian Institute of Astrophysics, Bangalore, 1988)
    The role of Our Sun as a valuable astrophysical laboratory for testing theories of stellar physics is highlighted. The state of our knowledge concerning the solar interior and the possible probes for gaining insight into ...
  • HR3040- on the Am track ? 
    Sreedhar Rao, S; Raghavender Rao, C; Kilambi, G. C (Astronomical Society of India, 1999)
    HR 3040 (HD 63589) exhibits pseudo-luminosity effects similar to many a main-sequence Am star, especially a strong Sr II 4077 line indicating a higher luminosity class. Its K-line matches that of A3 V, violet and blue ...
  • The Hubble constant 
    Narlikar, J. V (Astronomical Society of India, 1996)
    In this talk the history of Hubble's constant is reviewed from the discovery of the velocity-distance relation to the present day measurements with the Hubble Space Telescope. The problems encountered in fixing the true ...

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