TOWARD UNDERSTANDING THE B[e] PHENOMENON. III. PROPERTIES OF THE OPTICAL COUNTERPART OF IRAS 00470+6429

Journal Article · Mon Jul 20 00:00:00 EDT 2009 · Astrophysical Journal

DOI:https://doi.org/10.1088/0004-637X/700/1/209; COUNTRY OF INPUT: INTERNATIONAL ATOMIC ENERGY AGENCY (IAEA)· OSTI ID:21313889

Miroshnichenko, A S ^[1]; Chentsov, E L; Klochkova, V G ^[2]; Zharikov, S V ^[3]; Grankin, K N ^[4]; Kusakin, A V ^[5]; Gandet, T L ^[6]; Klingenberg, G ^[7]; Kildahl, S ^[8]; Rudy, R J; Lynch, D K; Venturini, C C; Mazuk, S ^[9]; Puetter, R C ^[10]; Perry, R B ^[11]; Carciofi, A C ^[12]; Bjorkman, K S ^[13]; Gray, R O ^[14]; Bernabei, S ^[15]

---

1. Department of Physics and Astronomy, University of North Carolina at Greensboro, Greensboro, NC 27402 (United States)
2. Special Astrophysical Observatory of the Russian Academy of Sciences, Nizhnyj Arkhyz, 369167 (Russian Federation)
3. Instituto de AstronomIa, Universidad Nacional Autonoma de Mexico, Apartado Postal 877, 22830, Ensenada, Baja California (Mexico)
4. Crimean Astrophysical Observatory, Nauchny, Crimea 334413 (Ukraine)
5. Sternberg Astronomical Institute, Universitetskij pr. 13, Moscow (Russian Federation)
6. Lizard Hollow Observatory, P.O. Box 89175, Tucson, AZ 85752-9175 (United States)
7. Bossmo Observatory, Mo i Rana (Norway)
8. Haugveien 1G 3300, Hokksund (Norway)
9. Aerospace Corporation, M2/266, P.O. Box 92957, Los Angeles, CA 90009 (United States)
10. University of California, San Diego, 9500 Gilman Dr., La Jolla, CA 92093 (United States)
11. Science Support Office, M/S 160, NASA Langley Research Center, Hampton, VA 23681 (United States)
12. Instituto de Astronomia, Geofisica e Ciencias Atmosfericas, Universidade de Sao Paulo, Rua do Matao 1226, Cidade Universitaria, Sao Paulo, SP 05508-900 (Brazil)
13. Ritter Observatory, Department of Physics and Astronomy, University of Toledo, Toledo, OH 43606-3390 (United States)
14. Department of Physics and Astronomy, Appalachian State University, Boone, NC 28608 (United States)
15. INAF-Osservatorio Astronomico di Bologna, Via Ranzani 1, 40127 Bologna (Italy)

FS CMa type stars are a group of Galactic objects with the B[e] phenomenon. They exhibit strong emission-line spectra and infrared excesses, which are most likely due to recently formed circumstellar dust. The group content and identification criteria were described in the first two papers of the series. In this paper we report our spectroscopic and photometric observations of the optical counterpart of IRAS 00470+6429 obtained in 2003-2008. The optical spectrum is dominated by emission lines, most of which have P Cyg type profiles. We detected significant brightness variations, which may include a regular component, and variable spectral line profiles in both shape and position. The presence of a weak Li I 6708 A line in the spectrum suggests that the object is most likely a binary system with a B2-B3 spectral-type primary companion of a luminosity log L/L {sub sun} = 3.9 {+-} 0.3 and a late-type secondary companion. We estimate a distance toward the object to be 2.0 {+-} 0.3 kpc from the Sun.

• OSTI ID: 21313889
• Journal Information: Astrophysical Journal, Vol. 700, Issue 1; Other Information: DOI: 10.1088/0004-637X/700/1/209; Country of input: International Atomic Energy Agency (IAEA); ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

99 GENERAL AND MISCELLANEOUS//MATHEMATICS, COMPUTING, AND INFORMATION SCIENCE
BRIGHTNESS
DISTANCE
DUSTS
EMISSION
LUMINOSITY
MATTER
SPECTRA
SUN