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Titolo:
OBSERVATIONS OF THE VELOCITY-FIELD OF NGC-4051
Autore:
KANEKO N; AOKI K; KOSUGI G; OHTANI H; YOSHIDA M; TOYAMA K; SATOH T; SASAKI M;
Indirizzi:
HOKKAIDO UNIV,FAC SCI,DEPT PHYS SAPPORO HOKKAIDO 060 JAPAN KYOTO UNIV,FAC SCI,DEPT ASTRON KYOTO 60601 JAPAN HOKKAIDO INFORMAT UNIV EBETSU HOKKAIDO 069 JAPAN KURIYAMA HIGH SCH KURIYAMA HOKKAIDO 06915 JAPAN SHIMONOSEKI CITY UNIV SHIMONOSEKI YAMAGUCHI 751 JAPAN NATL ASTRON OBSERV,OKAYAMA ASTROPHYS OBSERV KAMOGATA OKAYAMA 71902 JAPAN
Titolo Testata:
The Astronomical journal
fascicolo: 1, volume: 114, anno: 1997,
pagine: 94 - 101
SICI:
0004-6256(1997)114:1<94:OOTVON>2.0.ZU;2-X
Fonte:
ISI
Lingua:
ENG
Soggetto:
RAY SPECTRAL VARIABILITY; EMISSION-LINE REGION; SEYFERT-GALAXIES; ROTATIONAL PROPERTIES; NGC-4051; MODELS;
Tipo documento:
Article
Natura:
Periodico
Settore Disciplinare:
Science Citation Index Expanded
Citazioni:
38
Recensione:
Indirizzi per estratti:
Citazione:
N. Kaneko et al., "OBSERVATIONS OF THE VELOCITY-FIELD OF NGC-4051", The Astronomical journal, 114(1), 1997, pp. 94-101

Abstract

Observations of the velocity field of the Seyfert galaxy NGC 4051 were made using 1.88 m reflector of Okayama Astrophysical Observatory. For 106 H II and nuclear regions in 17 long-slit spectra (P,A. =110 degrees) which covered almost an entire optical image of similar to 3'x3',we measured H alpha to present the velocities in tabular form. The emission region is rather annular, and the observed H alpha velocities are gradually increasing with distance from the center to a radius of similar to 90'' with no maximum or hat part. Analyses give V-h = 697 +/- 11 km s(-1) and phi = 130 degrees +/- 14 degrees for the heliocentric systemic velocity and the major axis position angle, respectively. Comparison shows that the H alpha velocity structure is consistent withthe Hr observations of Liszt & Dickey (1995, AJ, 110, 998). However, the rotation curve corrected for the galaxy inclination (i = 37 degrees) is different from any of the synthetic rotation curves of Rubin et al. (1985, ApJ, 289, 81) both in the form of rotation curve and in theabsolute magnitude of galaxies. (C) 1997 American Astronomical Society.

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Documento generato il 03/07/20 alle ore 01:18:25