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A.Y. Kniazev18
- D. Engels2
- S.A. Pustilnik18
- A.V. Ugryumov18
- T.F. Kniazeva1
- A.G. Pramsky1
- N. Brosch3
- H.-J. Hagen2
- U. Hopp4
- Y.I. Izotov5
- V.A. Lipovetsky1
- J. Masegosa6
- I. Márquez6
- J.-M. Martin7
Special Astrophysical Observatory, Nizhnij Arkhyz, Karachai-Circessia, 369167, Russia - Hamburger Sternwarte, Gojenbergsweg 112, D-21029 Hamburg, Germany - Wise Observatory, Tel-Aviv University, Tel-Aviv 69978, Israel - Universitätssternwarte München, Scheiner Str. 1, D-81679 München, Germany - Main Astronomical Observatory, Goloseevo, Kiev-127, 03680, Ukraine - Instituto de Astrofisica de Andalucia, CSIC, Aptdo. 3004, 18080, Granada, Spain - Département de Radioastronomie ARPEGES, Observatoire de Paris, F-92195 Meudon Cedex, France - Isaac Newton Institute of Chile, SAO Branch
Received ; Accepted
We present the fourth list with results of the
Hamburg/SAO Survey for Emission-Line Galaxies (HSS hereafter, SAO -
Special Astrophysical Observatory, Russia). The list is a result of
the follow-up spectroscopy conducted with the 6m SAO RAS telescope
in 1998, 1999 and 2000. The data of this snap-shot spectroscopy
survey confirmed 127 emission-line objects out of 176 observed
candidates and allowed their quantitative spectral classification. We
could classify 76 emission-line objects as BCG/H II galaxies or
probable BCGs, 8 - as QSOs, 2 - as Seyfert galaxies, 2 - as
super-associations in a subluminous spiral and an irregular galaxy,
and 37 as low-excitation objects - either starburst nuclei (SBN), or
dwarf amorphous nuclei starburst galaxies (DANS). We could not
classify 2 ELGs. Furthermore, for 5 galaxies we did not detect any
significant emission lines.
For 91
emission-line galaxies, the redshifts and/or line intensities are
determined for the first time. Of the remaining 28
previously known ELGs we give either improved data on the line
intensities or some independent measurements.
The candidates were taken from three different samples selected by
different criteria. Among our first priority candidates we achieved
a detection rate of emission-line objects (ELGs + QSOs) of 68%,
among which 51% are BCGs. Observations of a random selected sample
among our second priority candidates showed that only 10% are
BCGs. We found that the confirmed BCGs have usually a blue colour
((B-R) < 10) and a non-stellar appearance in the APM database.
Our third sample is comprised of second priority candidates fulfilling
these criteria derived from the APM. Follow-up spectroscopy of a
small subsample indicates that the expected detection rate for BCGs
is
40%.
surveys - galaxies: fundamental parameters - galaxies: distances and redshifts - galaxies: starburst - galaxies: compact - quasars: redshifts