<?xml version="1.0" encoding="UTF-8"?>
<!DOCTYPE dataset SYSTEM "http://tarantella.gsfc.nasa.gov/xml/dataset_048.dtd">
<dataset subject="astronomy" xmlns:xlink="http://www.w3.org/XML/XLink/0.9">
	<title>Amendment of our method for deriving stellar membership of an open cluster</title>
	<altname type="ADC">J/AJ/109/1903</altname>
		<altname type="CDS">J/AJ/109/1903</altname>
		<altname type="brief">Membership to cluster IC 4756</altname>
	<reference>
		<source>
<journal>
	<title>Amendment of our method for deriving stellar membership of an open cluster</title>
	<author>
			<initial>M</initial>
			<lastName>Missana</lastName></author>
	<author>
			<initial>N</initial>
			<lastName>Missana</lastName></author>
	<name>Astron. J.</name>
	<volume>109</volume>
	<pageno>1903</pageno>
		<date>
			<year>1995</year></date>
	<bibcode>1995AJ....109.1903M</bibcode></journal></source></reference>
	<keywords parentListURL="http://messier.gsfc.nasa.gov/xml/keywordlists/adc_keywords.html">
			<keyword xlink:href="Clusters_open.html">Clusters, open</keyword></keywords>
	<descriptions>
				<abstract>
					<para>
    Our method for determining statistically the members of an open
    cluster by means of the proper motions (Missana et al.,
    (1990AJ....100.1850M) is amended and its validity is verified by
    applying it to the cluster IC 4756 with the data given by Herzog et
    al. (1975A&amp;AS...19..211H), adding nothing to their results. In the
    computation of the dispersion ellipses of the samples and of the
    {chi}^2^ for deriving the significance levels, the weights of the
    proper motions have been taken into account. The results obtained by
    the criterion of the {chi}^2^ and those obtained by Herzog et al. by
    the criterion of the maximum likelihood of Sanders
    (1971A&amp;A....14..226S) are concordant.</para></abstract>
                        <details>
	<astroObjects>
		
			<astroObject><name>IC 4756</name><name>C 1836+054</name><position><ra>18 39.0 </ra><dec>+05 28 </dec></position></astroObject></astroObjects></details></descriptions>
	<tableHead>
		<tableLinks>
				<tableLink xlink:href="table1">
	<title>Membership probabilities to IC 4756</title></tableLink></tableLinks>
	<fields>
		<field>
			<name>Star</name>
			<definition>Number of the star in Herzog et al.
                                    (1975A&amp;AS...19..211H)</definition>
			<units>---</units></field>
		<field>
			<name>Mi</name>
			<definition>Membership probability P(C\A).
	<footnote footnoteId="???"><para>number=1</para>
			<para>Probable member if P(C/A)>=0.5.
          See Missana et al., 1990AJ....100.1850M, for more details.
</para></footnote></definition>
			<units>---</units></field>
		<field>
			<name>n_Mi</name>
			<definition>* and &amp; indicate that the star belongs to
                                   the set of 174 and 109 cluster members
                                   respectively.</definition>
			<units>---</units></field>
		<field>
			<name>HS</name>
			<definition>Membership probability according to
                                        Herzog et al. ((1975A&amp;AS...19..211H)</definition>
			<units>---</units></field>
		<field>
			<name>MF</name>
			<definition>Cluster member (M) or field star (F) as
                                        per phot. estimates by Herzog et al.</definition>
			<units>---</units></field>
		<field>
			<name>B</name>
			<definition>B: Blue straggler.</definition>
			<units>---</units></field></fields></tableHead>
	
	<history>
		<ingest>
	
			<creator>
				<lastName>James Marcout, Patricia Bauer</lastName>
				<affiliation>CDS</affiliation></creator>
	<date>
		<year>1997</year><month>Apr</month><day>07</day></date></ingest>
		
		<revisions>
	<revision>
		<creator>
			<lastName>UNKNOWN</lastName></creator>
		<date><year>UNKNOWN</year></date>
		<para> Prepared via OCR at CDS.</para></revision></revisions></history>
	<identifier>J_AJ_109_1903.xml</identifier></dataset>
