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17 results on '"H. BLUMER"'

1. The Green Bank North Celestial Cap Pulsar Survey. V. Pulsar Census and Survey Sensitivity.

Author

A. E. McEwen, R. Spiewak, J. K. Swiggum, D. L. Kaplan, W. Fiore, G. Y. Agazie, H. Blumer, P. Chawla, M. DeCesar, V. M. Kaspi, V. I. Kondratiev, M. LaRose, L. Levin, R. S. Lynch, M. McLaughlin, M. Mingyar, H. Al Noori, S. M. Ransom, M. S. E. Roberts, and A. Schmiedekamp

Subjects
PULSAR detection, RADIO interference, PULSARS, ACTINIC flux, PARAMETERS (Statistics), SIGNAL-to-noise ratio
Abstract

The Green Bank North Celestial Cap (GBNCC) pulsar survey will cover the entire northern sky (δ > −40°) at 350 MHz, and is one of the most uniform and sensitive all-sky pulsar surveys to date. We have created a pipeline to reanalyze GBNCC survey data to take a 350 MHz census of all pulsars detected by the survey, regardless of their discovery survey. Of the 1413 pulsars in the survey region, we were able to recover 670. For these we present measured signal-to-noise ratios (S/N), flux densities, pulse widths, profiles, and where appropriate, refined measurements of dispersion measures (DMs) (656 out of 670) and new or improved spectral indices (339 out of 670 total, 47 new, 292 improved). We also measure the period-pulse width relation at 350 MHz to scale as . Detection scans for several hundred sources were reanalyzed in order to inspect pulsars’ single pulse behavior and 223 were found to exhibit evidence of nulling. With a detailed analysis of measured and expected S/N values and the evolving radio frequency interference environment at 350 MHz, we assess the GBNCC survey’s sensitivity as a function of spin period, DM, and sky position. We find the sky-averaged limiting flux density of the survey to be 0.74 mJy. Combining this analysis with PsrPopPy pulsar population simulations, we predict 60/5 nonrecycled/MSP discoveries in the survey’s remaining 21,000 pointings, and we begin to place constraints on population model parameters. [ABSTRACT FROM AUTHOR]

Published
2020
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2. The NANOGrav 12.5 yr Data Set: The Frequency Dependence of Pulse Jitter in Precision Millisecond Pulsars.

Author

M. T. Lam, M. A. McLaughlin, Z. Arzoumanian, H. Blumer, P. R. Brook, H. T. Cromartie, P. B. Demorest, M. E. DeCesar, T. Dolch, J. A. Ellis, R. D. Ferdman, E. C. Ferrara, E. Fonseca, N. Garver-Daniels, P. A. Gentile, M. L. Jones, D. R. Lorimer, R. S. Lynch, C. Ng, and D. J. Nice

Subjects
PULSARS, GRAVITATIONAL wave astronomy, SIGNAL-to-noise ratio, SCINTILLATION of stars, SCATTERING (Physics)
Abstract

Low-frequency gravitational-wave experiments require the highest timing precision from an array of the most stable millisecond pulsars. Several known sources of noise on short timescales in single radio pulsar observations are well described by a simple model of three components: template fitting from a finite signal-to-noise ratio, pulse phase/amplitude jitter from single-pulse stochasticity, and scintillation errors from short-timescale interstellar scattering variations. Currently template-fitting errors dominate, but as radio telescopes push toward higher signal-to-noise ratios, jitter becomes the next dominant term for most millisecond pulsars. Understanding the statistics of jitter becomes crucial for properly characterizing arrival time uncertainties. We characterize the radio frequency dependence of jitter using data on 48 pulsars in the North American Nanohertz Observatory for Gravitational Waves timing program. We detect significant jitter in 43 of the pulsars and test several functional forms for its frequency dependence; we find significant frequency dependence for 30 pulsars. We find moderate correlations of rms jitter with pulse width (R = 0.62) and number of profile components (R = 0.40); the single-pulse rms jitter is typically ≈1% of pulse phase. The average frequency dependence for all pulsars using a power-law model has index −0.42. We investigate the jitter variations for the interpulse of PSR B1937+21 and find no significant deviations from the main pulse rms jitter. We also test the time variation of jitter in two pulsars and find that systematics likely bias the results for high-precision pulsars. Pulsar timing array analyses must properly model jitter as a significant component of the noise within the detector. [ABSTRACT FROM AUTHOR]

Published
2019
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3. PSR J2234+0611: A New Laboratory for Stellar Evolution.

Author

K. Stovall, P. C. C. Freire, J. Antoniadis, M. Bagchi, J. S. Deneva, N. Garver-Daniels, J. G. Martinez, M. A. McLaughlin, Z. Arzoumanian, H. Blumer, P. R. Brook, H. T. Cromartie, P. B. Demorest, M. E. DeCesar, T. Dolch, J. A. Ellis, R. D. Ferdman, E. C. Ferrara, E. Fonseca, and P. A. Gentile

Subjects
WHITE dwarf stars, STELLAR evolution, PULSARS, STELLAR parallax, STELLAR orbits, RADIAL velocity of stars, STELLAR mass, STELLAR atmospheres
Abstract

We report the timing results for PSR J2234+0611, a 3.6 ms pulsar in a 32 day, eccentric (e = 0.13) orbit with a helium white dwarf. The precise timing and eccentric nature of the orbit allow measurements of an unusual number of parameters: (a) a precise proper motion of 27.10(3) mas yr−1 and a parallax of 1.05(4) mas resulting in a pulsar distance of 0.95(4) kpc; enabling an estimate of the transverse velocity, 123(5) km s−1. Together with previously published spectroscopic measurements of the systemic radial velocity, this allows a 3D determination of the system’s velocity; (b) precise measurements of the rate of advance of periastron yields a total system mass of M⊙; (c) a Shapiro delay measurement, h3 = 82 ± 14 ns, despite the orbital inclination not being near 90°; combined with the measurement of the total mass yields a pulsar mass of and a companion mass of (d) we measure precisely the secular variation of the projected semimajor axis and detect a significant annual orbital parallax; together these allow a determination of the 3D orbital geometry of the system, including an unambiguous orbital inclination () and a position angle for the line of nodes (). We discuss the component masses to investigate the hypotheses previously advanced to explain the origin of eccentric MSPs. The unprecedented determination of the 3D position, motion, and orbital orientation of the system, plus the precise pulsar and WD masses and the latter’s optical detection make this system a unique test of our understanding of white dwarfs and their atmospheres. [ABSTRACT FROM AUTHOR]

Published
2019
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4. A Second Chromatic Timing Event of Interstellar Origin toward PSR J1713+0747.

Author

M. T. Lam, J. A. Ellis, G. Grillo, M. L. Jones, J. S. Hazboun, P. R. Brook, J. E. Turner, S. Chatterjee, J. M. Cordes, T. J. W. Lazio, M. E. DeCesar, Z. Arzoumanian, H. Blumer, H. T. Cromartie, P. B. Demorest, T. Dolch, R. D. Ferdman, E. C. Ferrara, E. Fonseca, and N. Garver-Daniels

Subjects
INTERSTELLAR medium, ASTROPHYSICS, DISPERSION (Chemistry), SOLAR radio emission, RADIO pulse time modulation
Abstract

The frequency dependence of radio pulse arrival times provides a probe of structures in the intervening media. Demorest et al. was the first to show a short-term (∼100–200 days) reduction in the electron content along the line of sight to PSR J1713+0747 in data from 2008 (approximately MJD 54750) based on an apparent dip in the dispersion measure of the pulsar. We report on a similar event in 2016 (approximately MJD 57510), with average residual pulse-arrival times ≈−3.0, −1.3, and −0.7 μs at 820, 1400, and 2300 MHz, respectively. Timing analyses indicate possible departures from the standard ν−2 dispersive-delay dependence. We discuss and rule out a wide variety of potential interpretations. We find the likeliest scenario to be lensing of the radio emission by some structure in the interstellar medium, which causes multiple frequency-dependent pulse arrival-time delays. [ABSTRACT FROM AUTHOR]

Published
2018
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5. Ultrahigh Energy Neutrinos at the Pierre Auger Observatory

Author

P. Abreu, M. Aglietta, M. Ahlers, E. J. Ahn, I. F. M. Albuquerque, D. Allard, I. Allekotte, J. Allen, P. Allison, A. Almela, J. Alvarez Castillo, J. Alvarez-Muñiz, R. Alves Batista, M. Ambrosio, A. Aminaei, L. Anchordoqui, S. Andringa, T. Antičić, C. Aramo, E. Arganda, F. Arqueros, H. Asorey, P. Assis, J. Aublin, M. Ave, M. Avenier, G. Avila, T. Bäcker, A. M. Badescu, M. Balzer, K. B. Barber, A. F. Barbosa, R. Bardenet, S. L. C. Barroso, B. Baughman, J. Bäuml, J. J. Beatty, B. R. Becker, K. H. Becker, A. Bellétoile, J. A. Bellido, S. BenZvi, C. Berat, X. Bertou, P. L. Biermann, P. Billoir, F. Blanco, M. Blanco, C. Bleve, H. Blümer, M. Boháčová, D. Boncioli, C. Bonifazi, R. Bonino, N. Borodai, J. Brack, I. Brancus, P. Brogueira, W. C. Brown, R. Bruijn, P. Buchholz, A. Bueno, R. E. Burton, K. S. Caballero-Mora, B. Caccianiga, L. Caramete, R. Caruso, A. Castellina, O. Catalano, G. Cataldi, L. Cazon, R. Cester, J. Chauvin, S. H. Cheng, A. Chiavassa, J. A. Chinellato, J. Chirinos Diaz, J. Chudoba, M. Cilmo, R. W. Clay, M. R. Coluccia, R. Conceição, F. Contreras, H. Cook, M. J. Cooper, J. Coppens, A. Cordier, S. Coutu, C. E. Covault, A. Creusot, A. Criss, J. Cronin, A. Curutiu, S. Dagoret-Campagne, R. Dallier, B. Daniel, S. Dasso, K. Daumiller, B. R. Dawson, R. M. de Almeida, M. De Domenico, C. De Donato, S. J. de Jong, G. De La Vega, W. J. M. de Mello Junior, J. R. T. de Mello Neto, I. De Mitri, V. de Souza, K. D. de Vries, L. del Peral, M. del Río, O. Deligny, H. Dembinski, N. Dhital, C. Di Giulio, M. L. Díaz Castro, P. N. Diep, F. Diogo, C. Dobrigkeit, W. Docters, J. C. D'Olivo, P. N. Dong, A. Dorofeev, J. C. dos Anjos, M. T. Dova, D. D'Urso, I. Dutan, J. Ebr, R. Engel, M. Erdmann, C. O. Escobar, J. Espadanal, A. Etchegoyen, P. Facal San Luis, H. Falcke, G. Farrar, A. C. Fauth, N. Fazzini, A. P. Ferguson, B. Fick, A. Filevich, A. Filipčič, S. Fliescher, C. E. Fracchiolla, E. D. Fraenkel, O. Fratu, U. Fröhlich, B. Fuchs, R. Gaior, R. F. Gamarra, S. Gambetta, B. García, S. T. Garcia Roca, D. Garcia-Gamez, D. Garcia-Pinto, A. Gascon Bravo, H. Gemmeke, P. L. Ghia, M. Giller, J. Gitto, H. Glass, M. S. Gold, G. Golup, F. Gomez Albarracin, M. Gómez Berisso, P. F. Gómez Vitale, P. Gonçalves, J. G. Gonzalez, B. Gookin, A. Gorgi, P. Gouffon, E. Grashorn, S. Grebe, N. Griffith, M. Grigat, A. F. Grillo, Y. Guardincerri, F. Guarino, G. P. Guedes, P. Hansen, D. Harari, T. A. Harrison, J. L. Harton, A. Haungs, T. Hebbeker, D. Heck, A. E. Herve, C. Hojvat, N. Hollon, V. C. Holmes, P. Homola, J. R. Hörandel, P. Horvath, M. Hrabovský, D. Huber, T. Huege, A. Insolia, F. Ionita, A. Italiano, C. Jarne, S. Jiraskova, M. Josebachuili, K. Kadija, K. H. Kampert, P. Karhan, P. Kasper, I. Katkov, B. Kégl, B. Keilhauer, A. Keivani, J. L. Kelley, E. Kemp, R. M. Kieckhafer, H. O. Klages, M. Kleifges, J. Kleinfeller, J. Knapp, D.-H. Koang, K. Kotera, N. Krohm, O. Krömer, D. Kruppke-Hansen, F. Kuehn, D. Kuempel, J. K. Kulbartz, N. Kunka, G. La Rosa, C. Lachaud, D. LaHurd, L. Latronico, R. Lauer, P. Lautridou, S. Le Coz, M. S. A. B. Leão, D. Lebrun, P. Lebrun, M. A. Leigui de Oliveira, A. Letessier-Selvon, I. Lhenry-Yvon, K. Link, R. López, A. Lopez Agüera, K. Louedec, J. Lozano Bahilo, L. Lu, A. Lucero, M. Ludwig, H. Lyberis, M. C. Maccarone, C. Macolino, S. Maldera, D. Mandat, P. Mantsch, A. G. Mariazzi, J. Marin, V. Marin, I. C. Maris, H. R. Marquez Falcon, G. Marsella, D. Martello, L. Martin, H. Martinez, O. Martínez Bravo, H. J. Mathes, J. Matthews, J. A. J. Matthews, G. Matthiae, D. Maurel, D. Maurizio, P. O. Mazur, G. Medina-Tanco, M. Melissas, D. Melo, E. Menichetti, A. Menshikov, P. Mertsch, C. Meurer, S. Mićanović, M. I. Micheletti, I. A. Minaya, L. Miramonti, L. Molina-Bueno, S. Mollerach, M. Monasor, D. Monnier Ragaigne, F. Montanet, B. Morales, C. Morello, E. Moreno, J. C. Moreno, M. Mostafá, C. A. Moura, M. A. Muller, G. Müller, M. Münchmeyer, R. Mussa, G. Navarra, J. L. Navarro, S. Navas, P. Necesal, L. Nellen, A. Nelles, J. Neuser, P. T. Nhung, M. Niechciol, L. Niemietz, N. Nierstenhoefer, D. Nitz, D. Nosek, L. Nožka, J. Oehlschläger, A. Olinto, M. Ortiz, N. Pacheco, D. Pakk Selmi-Dei, M. Palatka, J. Pallotta, N. Palmieri, G. Parente, E. Parizot, A. Parra, S. Pastor, T. Paul, M. Pech, J. Pękala, R. Pelayo, I. M. Pepe, L. Perrone, R. Pesce, E. Petermann, S. Petrera, A. Petrolini, Y. Petrov, C. Pfendner, R. Piegaia, T. Pierog, P. Pieroni, M. Pimenta, V. Pirronello, M. Platino, M. Plum, V. H. Ponce, M. Pontz, A. Porcelli, P. Privitera, M. Prouza, E. J. Quel, S. Querchfeld, J. Rautenberg, O. Ravel, D. Ravignani, B. Revenu, J. Ridky, S. Riggi, M. Risse, P. Ristori, H. Rivera, V. Rizi, J. Roberts, W. Rodrigues de Carvalho, G. Rodriguez, I. Rodriguez Cabo, J. Rodriguez Martino, J. Rodriguez Rojo, M. D. Rodríguez-Frías, G. Ros, J. Rosado, T. Rossler, M. Roth, B. Rouillé-d'Orfeuil, E. Roulet, A. C. Rovero, C. Rühle, A. Saftoiu, F. Salamida, H. Salazar, F. Salesa Greus, G. Salina, F. Sánchez, C. E. Santo, E. Santos, E. M. Santos, F. Sarazin, B. Sarkar, S. Sarkar, R. Sato, N. Scharf, V. Scherini, H. Schieler, P. Schiffer, A. Schmidt, O. Scholten, H. Schoorlemmer, J. Schovancova, P. Schovánek, F. Schröder, S. Schulte, D. Schuster, S. J. Sciutto, M. Scuderi, A. Segreto, M. Settimo, A. Shadkam, R. C. Shellard, I. Sidelnik, G. Sigl, O. Sima, A. Śmiałkowski, R. Šmída, G. R. Snow, P. Sommers, J. Sorokin, H. Spinka, R. Squartini, Y. N. Srivastava, S. Stanic, J. Stapleton, J. Stasielak, M. Stephan, A. Stutz, F. Suarez, T. Suomijärvi, A. D. Supanitsky, T. Šuša, M. S. Sutherland, J. Swain, Z. Szadkowski, M. Szuba, A. Tapia, M. Tartare, O. Taşcău, R. Tcaciuc, N. T. Thao, D. Thomas, J. Tiffenberg, C. Timmermans, W. Tkaczyk, C. J. Todero Peixoto, G. Toma, L. Tomankova, B. Tomé, A. Tonachini, P. Travnicek, D. B. Tridapalli, G. Tristram, E. Trovato, M. Tueros, R. Ulrich, M. Unger, M. Urban, J. F. Valdés Galicia, I. Valiño, L. Valore, A. M. van den Berg, E. Varela, B. Vargas Cárdenas, J. R. Vázquez, R. A. Vázquez, D. Veberič, V. Verzi, J. Vicha, M. Videla, L. Villaseñor, H. Wahlberg, P. Wahrlich, O. Wainberg, D. Walz, A. A. Watson, M. Weber, K. Weidenhaupt, A. Weindl, F. Werner, S. Westerhoff, B. J. Whelan, A. Widom, G. Wieczorek, L. Wiencke, B. Wilczyñska, H. Wilczyñski, M. Will, C. Williams, T. Winchen, M. Wommer, B. Wundheiler, T. Yamamoto, T. Yapici, P. Younk, G. Yuan, A. Yushkov, B. Zamorano Garcia, E. Zas, D. Zavrtanik, M. Zavrtanik, I. Zaw, A. Zepeda, Y. Zhu, M. Zimbres Silva, and M. Ziolkowski

Subjects
Physics, QC1-999
Abstract

The observation of ultrahigh energy neutrinos (UHEνs) has become a priority in experimental astroparticle physics. UHEνs can be detected with a variety of techniques. In particular, neutrinos can interact in the atmosphere (downward-going ν) or in the Earth crust (Earth-skimming ν), producing air showers that can be observed with arrays of detectors at the ground. With the surface detector array of the Pierre Auger Observatory we can detect these types of cascades. The distinguishing signature for neutrino events is the presence of very inclined showers produced close to the ground (i.e., after having traversed a large amount of atmosphere). In this work we review the procedure and criteria established to search for UHEνs in the data collected with the ground array of the Pierre Auger Observatory. This includes Earth-skimming as well as downward-going neutrinos. No neutrino candidates have been found, which allows us to place competitive limits to the diffuse flux of UHEνs in the EeV range and above.

Published
2013
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6. Searching for Gravitational Waves from Cosmological Phase Transitions with the NANOGrav 12.5-Year Dataset.

Author

Arzoumanian Z, Baker PT, Blumer H, Bécsy B, Brazier A, Brook PR, Burke-Spolaor S, Charisi M, Chatterjee S, Chen S, Cordes JM, Cornish NJ, Crawford F, Cromartie HT, DeCesar ME, Demorest PB, Dolch T, Ellis JA, Ferrara EC, Fiore W, Fonseca E, Garver-Daniels N, Gentile PA, Good DC, Hazboun JS, Holgado AM, Islo K, Jennings RJ, Jones ML, Kaiser AR, Kaplan DL, Kelley LZ, Key JS, Laal N, Lam MT, Lazio TJW, Lee VSH, Lorimer DR, Luo J, Lynch RS, Madison DR, McLaughlin MA, Mingarelli CMF, Mitridate A, Ng C, Nice DJ, Pennucci TT, Pol NS, Ransom SM, Ray PS, Shapiro-Albert BJ, Siemens X, Simon J, Spiewak R, Stairs IH, Stinebring DR, Stovall K, Sun JP, Swiggum JK, Taylor SR, Turner JE, Vallisneri M, Vigeland SJ, Witt CA, and Zurek KM

Abstract

We search for a first-order phase transition gravitational wave signal in 45 pulsars from the NANOGrav 12.5-year dataset. We find that the data can be modeled in terms of a strong first order phase transition taking place at temperatures below the electroweak scale. However, we do not observe any strong preference for a phase-transition interpretation of the signal over the standard astrophysical interpretation in terms of supermassive black hole mergers; but we expect to gain additional discriminating power with future datasets, improving the signal to noise ratio and extending the sensitivity window to lower frequencies. An interesting open question is how well gravitational wave observatories could separate such signals.

Published
2021
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7. The sequence and analysis of duplication-rich human chromosome 16.

Author

Martin J, Han C, Gordon LA, Terry A, Prabhakar S, She X, Xie G, Hellsten U, Chan YM, Altherr M, Couronne O, Aerts A, Bajorek E, Black S, Blumer H, Branscomb E, Brown NC, Bruno WJ, Buckingham JM, Callen DF, Campbell CS, Campbell ML, Campbell EW, Caoile C, Challacombe JF, Chasteen LA, Chertkov O, Chi HC, Christensen M, Clark LM, Cohn JD, Denys M, Detter JC, Dickson M, Dimitrijevic-Bussod M, Escobar J, Fawcett JJ, Flowers D, Fotopulos D, Glavina T, Gomez M, Gonzales E, Goodstein D, Goodwin LA, Grady DL, Grigoriev I, Groza M, Hammon N, Hawkins T, Haydu L, Hildebrand CE, Huang W, Israni S, Jett J, Jewett PB, Kadner K, Kimball H, Kobayashi A, Krawczyk MC, Leyba T, Longmire JL, Lopez F, Lou Y, Lowry S, Ludeman T, Manohar CF, Mark GA, McMurray KL, Meincke LJ, Morgan J, Moyzis RK, Mundt MO, Munk AC, Nandkeshwar RD, Pitluck S, Pollard M, Predki P, Parson-Quintana B, Ramirez L, Rash S, Retterer J, Ricke DO, Robinson DL, Rodriguez A, Salamov A, Saunders EH, Scott D, Shough T, Stallings RL, Stalvey M, Sutherland RD, Tapia R, Tesmer JG, Thayer N, Thompson LS, Tice H, Torney DC, Tran-Gyamfi M, Tsai M, Ulanovsky LE, Ustaszewska A, Vo N, White PS, Williams AL, Wills PL, Wu JR, Wu K, Yang J, Dejong P, Bruce D, Doggett NA, Deaven L, Schmutz J, Grimwood J, Richardson P, Rokhsar DS, Eichler EE, Gilna P, Lucas SM, Myers RM, Rubin EM, and Pennacchio LA

Subjects
Animals, Genes genetics, Genomics, Heterochromatin genetics, Humans, Molecular Sequence Data, Polymorphism, Genetic genetics, Sequence Analysis, DNA, Synteny genetics, Chromosomes, Human, Pair 16 genetics, Gene Duplication, Physical Chromosome Mapping
Abstract

Human chromosome 16 features one of the highest levels of segmentally duplicated sequence among the human autosomes. We report here the 78,884,754 base pairs of finished chromosome 16 sequence, representing over 99.9% of its euchromatin. Manual annotation revealed 880 protein-coding genes confirmed by 1,670 aligned transcripts, 19 transfer RNA genes, 341 pseudogenes and three RNA pseudogenes. These genes include metallothionein, cadherin and iroquois gene families, as well as the disease genes for polycystic kidney disease and acute myelomonocytic leukaemia. Several large-scale structural polymorphisms spanning hundreds of kilobase pairs were identified and result in gene content differences among humans. Whereas the segmental duplications of chromosome 16 are enriched in the relatively gene-poor pericentromere of the p arm, some are involved in recent gene duplication and conversion events that are likely to have had an impact on the evolution of primates and human disease susceptibility.

Published
2004
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10. Viral hepatitis.

Author

BLACKWELL C and BLUMER H

Subjects
Humans, Communicable Diseases, Hepatitis, Hepatitis A, Hepatitis, Viral, Human
Published
1955

15. Respiratory therapy for seasonal allergic rhinitis and asthma.

Author

BLUMER H, LEZNOFF A, CUA-LIM F, DELORME P, and ROSE B

Subjects
Adult, Female, Humans, Male, Allergens, Asthma, Pollen, Respiratory Therapy, Rhinitis, Allergic, Rhinitis, Allergic, Seasonal, Seasons
Abstract

Repository therapy with an emulsified antigen preparation for pollen asthma and hay fever was used over the past three years. Overall results indicate that the response in the majority of patients was as good as that obtained with conventional preseasonal or perennial treatment. Reactions were noted in four of the 15 patients so treated during the first year of study, in 25 of 58 patients treated in the second year, and in 11 of 175 treated in the final year. These varied from mild to severe systemic reactions, some of which required hospitalization. With improvement and modification of the technique, such as the administration of the antigen in two injections rather than in a single injection, the incidence and severity of reactions were markedly reduced. The procedure is not without hazard; it requires great care, and initial experience is best obtained in a hospital environment.

Published
1962

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