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9 results on '"D. Osip"'

1. Optical Spectroscopy of Type Ia Supernovae by the Carnegie Supernova Projects I and II

Author

N. Morrell, M. M. Phillips, G. Folatelli, M. D. Stritzinger, M. Hamuy, N. B. Suntzeff, E. Y. Hsiao, F. Taddia, C. R. Burns, P. Hoeflich, C. Ashall, C. Contreras, L. Galbany, J. Lu, A. L. Piro, J. Anais, E. Baron, A. Burrow, L. Busta, A. Campillay, S. Castellón, C. Corco, T. Diamond, W. L. Freedman, C. Gonzalez, K. Krisciunas, S. Kumar, S. E. Persson, J. Serón, M. Shahbandeh, S. Torres, S. A. Uddin, J. P. Anderson, C. Baltay, C. Gall, A. Goobar, E. Hadjiyska, S. Holmbo, M. Kasliwal, C. Lidman, G. H. Marion, P. A. Mazzali, P. Nugent, S. Perlmutter, G. Pignata, D. Rabinowitz, M. Roth, S. D. Ryder, B. J. Shappee, J. Vinkó, J. C. Wheeler, T. de Jaeger, P. Lira, M. T. Ruiz, J. A. Rich, J. L. Prieto, F. Di Mille, D. Osip, G. Blanc, and P. Palunas

Subjects
Supernovae, Spectroscopy, Astrophysics, QB460-466
Abstract

We present the second and final release of optical spectroscopy of Type Ia supernovae (SNe Ia) obtained during the first and second phases of the Carnegie Supernova Project (CSP-I and CSP-II). The newly released data consist of 148 spectra of 30 SNe Ia observed in the course of CSP-I and 234 spectra of 127 SNe Ia obtained during CSP-II. We also present 216 optical spectra of 46 historical SNe Ia, including 53 spectra of 30 SNe Ia observed by the Calán/Tololo Supernova Survey. We combine these observations with previously published CSP data and publicly available spectra to compile a large sample of measurements of spectroscopic parameters at maximum light, consisting of pseudo-equivalent widths and expansion velocities of selected features for 232 CSP and historical SNe Ia (including more than 1000 spectra). Finally, we review some of the strongest correlations between spectroscopic and photometric properties of SNe Ia. Specifically, we define two samples: one consisting of SNe Ia discovered by targeted searches (most of them CSP-I objects) and the other composed of SNe Ia discovered by untargeted searches, which includes most of the CSP-II objects. The analyzed correlations are similar for both samples. We find a larger incidence of SNe Ia belonging to the cool and broad-line Branch subtypes among the events discovered by targeted searches, shallow-silicon SNe Ia are present with similar frequencies in both samples, while core normal SNe Ia are more frequent in untargeted searches.

Published
2024
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4. The Cluster Ages Experiment (CASE) – IX. Analysis of four detached eclipsing binaries in the globular cluster NGC 3201

Author

M Rozyczka, I B Thompson, A Dotter, B Mazur, W Narloch, W Pych, K G Hełminiak, A Moharana, Y Beletsky, G S Burley, J L Marshall, N Morrell, D Osip, S A Shectman, R Bernstein, B Pilecki, and B Zgirski

Subjects
Space and Planetary Science, Astronomy and Astrophysics
Abstract

We use photometric and spectroscopic observations of four detached eclipsing binaries in the globular cluster NGC 3201 to derive masses, radii, and luminosities of the component stars. Spanning across almost three magnitudes in the colour–magnitude diagram, the components offer a unique possibility to test the theory of stellar evolution. Their masses, radii, and luminosities range from 0.66 to 0.84 M⊙, 0.68 to 2.46 R⊙, and 0.38 to 5.56 L⊙, respectively. The distance to the cluster measured from the distance moduli of the component stars amounts to 4.54$^{+0.11}_{-0.14}$ kpc and agrees with the recent estimate based on Gaia parallaxes. By comparing the M − R and M − L diagrams of the component stars and the colour–magnitude diagram of NGC 3201 to Dartmouth model isochrones, we estimate the most probable age of the cluster to be 11.5 ± 0.5 Gyr. This estimate is based on three binaries only, as the fourth one seems to evolve along a different path, probably due to non-standard chemical composition and/or history. We confirm the tendency, observed in earlier CASE papers, for the age indicated by the M − R diagram to be younger than that implied by the colour–magnitude diagram.

Published
2022
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5. Deep Photometry of GRB 041006 Afterglow: Hypernova Bump at Redshift z=0.716

Author

K. Z. Stanek, P. M. Garnavich, P. A. Nutzman, J. D. Hartman, A. Garg, K. Adelberger, P. Berlind, A. Z. Bonanos, M. L. Calkins, P. Challis, B. S. Gaudi, M. J. Holman, R. P. Kirshner, B. A. McLeod, D. Osip, T. Pimenova, T. H. Reiprich, W. Romanishin, T. Spahr, S. C. Tegler, and X. Zhao

Subjects
Physics, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Light curve, Redshift, Luminosity, Afterglow, Photometry (optics), Supernova, Space and Planetary Science, Hypernova, Gamma-ray burst
Abstract

We present deep optical photometry of the afterglow of gamma-ray burst (GRB) 041006 and its associated hypernova obtained over 65 days after detection (55 R-band epochs on 10 different nights). Our early data (t, ApJ Letters, accepted. Additional material available at ftp://cfa-ftp.harvard.edu/pub/kstanek/GRB041006/

Published
2005

6. Regression of Liver Steatosis Following Phosphatidylcholine Administration: A Review of Molecular and Metabolic Pathways Involved

Author

D. Osipova, K. Kokoreva, L. Lazebnik, E. Golovanova, Ch. Pavlov, A. Dukhanin, S. Orlova, and K. Starostin

Subjects
liver steatosis, essential phospholipids, mode of action, pharmacodynamics, phosphatydilcholine, nonalcoholic fatty liver, Therapeutics. Pharmacology, RM1-950
Abstract

Liver steatosis is a key pathology in non-alcoholic or metabolic associated fatty liver disease. Though largely ignored for decades it is currently becoming the focus of research in hepatology. It is important to consider its origin and current opportunities in terms of pharmacotherapy. Essential phospholipids (EPLs) rich in phosphatidylcholine (PCH) is a widely used treatment option for fatty liver disease, and there is a solid amount of consistent clinical evidence for the regression of steatosis after treatment with EPLs. As knowledge of PCH (a key component of EPLs) pharmacodynamics and mode of action driving this widely observed clinical effect is currently insufficient, we aimed to explore the potential molecular and metabolic pathways involved in the positive effects of PCH on steatosis regression.

Published
2022
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7. HATS-70b: A 13 MJ Brown Dwarf Transiting an A Star.

Author

G. Zhou, G. Á. Bakos, D. Bayliss, J. Bento, W. Bhatti, R. Brahm, Z. Csubry, N. Espinoza, J. D. Hartman, T. Henning, A. Jordán, L. Mancini, K. Penev, M. Rabus, P. Sarkis, V. Suc, M. de Val-Borro, J. E. Rodriguez, D. Osip, and L. Kedziora-Chudczer

Published
2019
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9. Deep Impact: observations from a worldwide Earth-based campaign.

Author

Meech KJ, Ageorges N, A'Hearn MF, Arpigny C, Ates A, Aycock J, Bagnulo S, Bailey J, Barber R, Barrera L, Barrena R, Bauer JM, Belton MJ, Bensch F, Bhattacharya B, Biver N, Blake G, Bockelée-Morvan D, Boehnhardt H, Bonev BP, Bonev T, Buie MW, Burton MG, Butner HM, Cabanac R, Campbell R, Campins H, Capria MT, Carroll T, Chaffee F, Charnley SB, Cleis R, Coates A, Cochran A, Colom P, Conrad A, Coulson IM, Crovisier J, deBuizer J, Dekany R, de Léon J, Dello Russo N, Delsanti A, DiSanti M, Drummond J, Dundon L, Etzel PB, Farnham TL, Feldman P, Fernández YR, Filipovic MD, Fisher S, Fitzsimmons A, Fong D, Fugate R, Fujiwara H, Fujiyoshi T, Furusho R, Fuse T, Gibb E, Groussin O, Gulkis S, Gurwell M, Hadamcik E, Hainaut O, Harker D, Harrington D, Harwit M, Hasegawa S, Hergenrother CW, Hirst P, Hodapp K, Honda M, Howell ES, Hutsemékers D, Iono D, Ip WH, Jackson W, Jehin E, Jiang ZJ, Jones GH, Jones PA, Kadono T, Kamath UW, Käufl HU, Kasuga T, Kawakita H, Kelley MS, Kerber F, Kidger M, Kinoshita D, Knight M, Lara L, Larson SM, Lederer S, Lee CF, Levasseur-Regourd AC, Li JY, Li QS, Licandro J, Lin ZY, Lisse CM, LoCurto G, Lovell AJ, Lowry SC, Lyke J, Lynch D, Ma J, Magee-Sauer K, Maheswar G, Manfroid J, Marco O, Martin P, Melnick G, Miller S, Miyata T, Moriarty-Schieven GH, Moskovitz N, Mueller BE, Mumma MJ, Muneer S, Neufeld DA, Ootsubo T, Osip D, Pandea SK, Pantin E, Paterno-Mahler R, Patten B, Penprase BE, Peck A, Petitas G, Pinilla-Alonso N, Pittichova J, Pompei E, Prabhu TP, Qi C, Rao R, Rauer H, Reitsema H, Rodgers SD, Rodriguez P, Ruane R, Ruch G, Rujopakarn W, Sahu DK, Sako S, Sakon I, Samarasinha N, Sarkissian JM, Saviane I, Schirmer M, Schultz P, Schulz R, Seitzer P, Sekiguchi T, Selman F, Serra-Ricart M, Sharp R, Snell RL, Snodgrass C, Stallard T, Stecklein G, Sterken C, Stüwe JA, Sugita S, Sumner M, Suntzeff N, Swaters R, Takakuwa S, Takato N, Thomas-Osip J, Thompson E, Tokunaga AT, Tozzi GP, Tran H, Troy M, Trujillo C, Van Cleve J, Vasundhara R, Vazquez R, Vilas F, Villanueva G, von Braun K, Vora P, Wainscoat RJ, Walsh K, Watanabe J, Weaver HA, Weaver W, Weiler M, Weissman PR, Welsh WF, Wilner D, Wolk S, Womack M, Wooden D, Woodney LM, Woodward C, Wu ZY, Wu JH, Yamashita T, Yang B, Yang YB, Yokogawa S, Zook AC, Zauderer A, Zhao X, Zhou X, and Zucconi JM

Subjects
Cosmic Dust, Jupiter, Organic Chemicals, Photometry, Meteoroids
Abstract

On 4 July 2005, many observatories around the world and in space observed the collision of Deep Impact with comet 9P/Tempel 1 or its aftermath. This was an unprecedented coordinated observational campaign. These data show that (i) there was new material after impact that was compositionally different from that seen before impact; (ii) the ratio of dust mass to gas mass in the ejecta was much larger than before impact; (iii) the new activity did not last more than a few days, and by 9 July the comet's behavior was indistinguishable from its pre-impact behavior; and (iv) there were interesting transient phenomena that may be correlated with cratering physics.

Published
2005
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