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J/A+A/509/A11 Halpha emission-line objects in SMC clusters (Martayan+, 2010)
The following files can be converted to FITS (extension .fit or fit.gz)
tablea1.dat tablea2.dat tableb1.dat tableb2.dat tableca.dat
tablecb.dat tablec9.dat
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Query from: http://vizier.cds.unistra.fr/viz-bin/VizieR?-source=J/A+A/509/A11
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drwxr-xr-x 17 cats archive 290 May 12 2015 [Up]
drwxr-xr-x 2 cats archive 4096 Jan 13 2023 [TAR file]
-rw-r--r-- 1 cats archive 542 Dec 19 2022 .message
-r--r--r-- 1 cats archive 19118 Mar 3 2011 ReadMe
-rw-r--r-- 1 cats archive 1010 Oct 2 2014 +footg5.gif
-rw-r--r-- 1 cats archive 2335 Oct 2 2014 +footg8.gif
-r--r--r-- 1 cats archive 7533 Nov 3 2009 tablea1.dat [txt] [txt.gz] [fits] [fits.gz] [html]
-r--r--r-- 1 cats archive 4859 Nov 5 2009 tablea2.dat [txt] [txt.gz] [fits] [fits.gz] [html]
-r--r--r-- 1 cats archive 16377 Nov 3 2009 tableb1.dat [txt] [txt.gz] [fits] [fits.gz] [html]
-r--r--r-- 1 cats archive 6712 Nov 3 2009 tableb2.dat [txt] [txt.gz] [fits] [fits.gz] [html]
-r--r--r-- 1 cats archive 4138 Mar 27 2010 tablec9.dat [txt] [txt.gz] [fits] [fits.gz] [html]
-r--r--r-- 1 cats archive 35378 Mar 27 2010 tableca.dat [txt] [txt.gz] [fits] [fits.gz] [html]
-r--r--r-- 1 cats archive 23044 Mar 27 2010 tablecb.dat [txt] [txt.gz] [fits] [fits.gz] [html]
Beginning of ReadMe :J/A+A/509/A11 Halpha emission-line objects in SMC clusters (Martayan+, 2010)
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A slitless spectroscopic survey for Halpha emission-line objects in SMC
clusters.
Martayan C., Baade D., Fabregat J.
<Astron. Astrophys. 509, A11 (2010)>
=2010A&A...509A..11M
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ADC_Keywords: Magellanic Clouds ; Stars, emission ; Photometry, UBVRI ;
Photometry, infrared
Keywords: stars: early-type - stars: emission-line, Be -
stars: fundamental parameters - stars: evolution - Magellanic Clouds -
catalogs
Abstract:
Slitless CCD spectra were obtained covering the bulk (about 3 square
degrees) of the Small Magellanic Cloud. For Halpha line-emission
twice as strong as the ambient continuum, the survey is complete to
spectral type B2/B3 on the main sequence. About 8120 spectra of 4437
stars were searched for emission lines in 84 open clusters, and 370
emission-line stars were found, among them at least 231 close to the
main sequence. For 176 of them, photometry is available from the OGLE
database. For comparison with a higher-metallicity environment, the
Galactic sample of the photometric Halpha survey by McSwain & Gies
(2005, Cat. J/ApJS/161/118) was used. Among early spectral
sub-types, Be stars are more frequent by a factor 3-5 in the SMC than
in the Galaxy. The distribution with spectral type is similar in both
galaxies, i.e., not strongly dependent on metallicity. The fraction of
Be stars does not seem to vary with local star density. The Be
phenomenon mainly sets in towards the end of the main-sequence
evolution (this trend may be more pronounced in the SMC); but some Be
stars already form with Be-star characteristics. In small subsamples
(such as single clusters), even if they appear identical, the fraction
of emission-line stars can deviate drastically from the mean. In all
probability, the fractional critical angular rotation rate, OMC, is
one of the main parameters governing the occurrence of the Be
phenomenon. If the Be character is only acquired during the course of
evolution, the key circumstance is the evolution of OMC, which is not
only dependent on metallicity but differently so for different mass
ranges. As a result, even if the Be phenomenon is driven basically by
a single parameter (namely OMC), it can assume a complex
multi-parametric appearance. The large cluster-to-cluster differences,
which seem stronger than all other variations, serve as a caveat that
this big picture may undergo significant second-order modulations
(e.g., pulsations, initial angular momentum, etc).
Description:
The observations were carried out on September 25 and 26, 2002 with
the Wide Field Imager (WFI) attached to the 2.2m MPG Telescope
at ESO's observatory on Cerro La Silla in Chile. In its slitless
spectroscopic mode, the WFI has a roughly circular field of view of
diameter 0.31deg, and the R50 grism has a dispersion of 54nm/mm
(0.811nm/pix); the nominal resolution at optimal focus and seeing
is 5.1nm at Halpha.