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Multisite spectroscopic and photometric observations of the pulsating sdB star PG 1605+072

Published online by Cambridge University Press:  12 April 2016

S.J. O’Toole ,
S. Falter ,
U. Heber ,
C.S. Jeffery ,
S. Dreizier ,
S.L. Schuh ,
the MSST  and
WET teams
S.J. O’Toole
Affiliation:
Dr Remeis-Sternwarte, Astronomisches Institut der Universität Erlangen-Nürnberg, Sternwartstr. 7, Bamberg D-96049, Germany
S. Falter
Affiliation:
Dr Remeis-Sternwarte, Astronomisches Institut der Universität Erlangen-Nürnberg, Sternwartstr. 7, Bamberg D-96049, Germany
U. Heber
Affiliation:
Dr Remeis-Sternwarte, Astronomisches Institut der Universität Erlangen-Nürnberg, Sternwartstr. 7, Bamberg D-96049, Germany
C.S. Jeffery
Affiliation:
Armagh Observatory, College Hill, Armagh BT61 9DG, Northern Ireland, UK
S. Dreizier
Affiliation:
Insitut für Astronomie und Astrophysik, Universität Tübingen, Sand 1, D-72076 Tübingen, Germany Universitätssternwarte, Universität Göttingen, Geismarlandstrasse 11, D-37083 Göttingen, Germany
S.L. Schuh
Affiliation:
Insitut für Astronomie und Astrophysik, Universität Tübingen, Sand 1, D-72076 Tübingen, Germany Universitätssternwarte, Universität Göttingen, Geismarlandstrasse 11, D-37083 Göttingen, Germany

Abstract

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We present the first results from the MultiSite Spectroscopic Telescope (MSST) observations of the sdBV star PG 1605+072. Pulsating sdB stars (V361 Hya stars) offer the chance to gain new insights into the formation and evolution of extreme Horizontal Branch stars using the tools of asteroseismology. PG 1605+072 is an outstanding object in its class, with the richest frequency spectrum, the longest periods, and the largest variations. The MSST campaign took place in 2002 May/June and we present here the massive data set, made up of 399 hr of photometry and 151 hr of spectroscopy. The overall aims of the project are to examine light/velocity amplitude ratios and phase differences, changes in equivalent width/line index, and λ-dependence of photometric amplitudes, and to use these properties for mode identification.

Type
Part 4. Early-type stars: B, A and F pulsators
Information
International Astronomical Union Colloquium , Volume 193: Variable Stars in the Local Group , 2004 , pp. 230 - 233
Copyright
Copyright © Astronomical Society of the Pacific 2004

References

Falter, S., Heber, U., Dreizier, S., et al. 2003 A&A, 401, 289 Google Scholar
Heber, U., et al. 2003, 13th European Workshop on White Dwarfs. NATO-ARW Workshop Series, p. 105 Google Scholar
Kilkenny, D., Koen, C., O’Donoghue, D., et al. 1999 MNRAS, 303, 525 Google Scholar
Koen, C., O’Donoghue, D., Kilkenny, D., et al. 1998 MNRAS, 296, 317 Google Scholar
O’Toole, S.J., Bedding, T.R., Kjeldsen, H., et al. 2000 ApJ, 537, L53 Google Scholar
OToole, S.J., Bedding, T.R., Kjeldsen, H., et al. 2002 MNRAS, 334, 471 Google Scholar
O’Toole, S.J., Jørgensen, M.A.S.G., Kjeldsen, H., et al. 2003 MNRAS, 340, 856 Google Scholar
Schuh, S.L., Dreizier, S., Deetjen, J.L., Göhler, E. 2003, Baltic Astron., 12, 167 Google Scholar
Woolf, V.M., Jeffery, C.S., Pollacco, D. 2002, MNRAS, 339, 497 Google Scholar