<?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>The Intrinsic Shape of NGC 3379</title>
	<altname type="ADC">J/AJ/108/111</altname>
		<altname type="CDS">J/AJ/108/111</altname>
		<altname type="brief">NGC 3379</altname>
	<reference>
		<source>
<journal>
	<title>The Intrinsic Shape of NGC 3379</title>
	<author>
			<initial>T</initial>
			<initial>S</initial>
			<lastName>Statler</lastName></author>
	<name>Astron. J.</name>
	<volume>108</volume>
	<pageno>111</pageno>
		<date>
			<year>1994</year></date>
	<bibcode>1994AJ....108..111S</bibcode></journal></source></reference>
	<keywords parentListURL="http://messier.gsfc.nasa.gov/xml/keywordlists/adc_keywords.html">
			<keyword xlink:href="Galaxies_optical.html">Galaxies, optical</keyword></keywords>
	<descriptions>
				<abstract>
					<para>
  Photometric and kinematic data from the literature are combined with
  new dynamical models to derive the intrinsic shape of the "standard"
  elliptical galaxy NGC 3379.  The parameters that are best constrained
  are the dynamical triaxiality T (essentially the triaxiality of the
  total mass distribution) and the short-to-long axis ratio of the light
  distribution c_L.  The inferred shape is given by a Bayesian
  probability distribution in the (T,c_L) plane.  Assuming a uniform
  prior, the most probable shape is oblate with a flattening of c_L=.87.
  The distribution is strongly non-Gaussian, however, and the expectation
  values, &lt;T>=.31, &lt;c_L>=.75, imply a flatter and more triaxial figure.
  The 68% highest posterior density region allows more triaxial shapes as
  long as they are fairly round, or flatter shapes as long as they are
  nearly oblate.  These results are essentially unchanged if the galaxy
  is assumed to rotate about its short axis, or if it is modeled as an S0
  with a negligible-mass disk rather than as an elliptical.  The
  suggestion of Capaccioli et al. [ApJ, 371, 535 (1991)] that NGC 3379 is
  a rather flat, triaxial S0 galaxy is found to be improbable at the 98%
  level; this conclusion is largely independent of the bulge-to-disk
  ratio or the relative rotation speeds of the two components.</para></abstract>
                        <details>
	<astroObjects>
		
			<astroObject><name>NGC 3379</name><name>UGC 5902</name><position><ra>10 47.8 </ra><dec>+12 35 </dec></position></astroObject></astroObjects></details></descriptions>
	<tableHead>
		<tableLinks>
				<tableLink xlink:href="table5.dat">
	<title>NGC 3379 point estimators, see Sect. 4.3 of the
                                printed paper for full details</title></tableLink></tableLinks>
	<fields>
		<field>
			<name>Index</name>
			<definition>Index to model parameters in tables 1,2,4</definition>
			<units>---</units></field>
		<field>
			<name>T</name>
			<definition>Expectation value of dynamical triaxiality</definition>
			<units>---</units></field>
		<field>
			<name>c_L</name>
			<definition>Exp. value of flattening of light distrib.</definition>
			<units>---</units></field>
		<field>
			<name>T_p</name>
			<definition>Most probable value of T</definition>
			<units>---</units></field>
		<field>
			<name>c_Lp</name>
			<definition>Most probable value of c_L</definition>
			<units>---</units></field>
		<field>
			<name>T_4</name>
			<definition>Maximum unprojected likelihood, T</definition>
			<units>---</units></field>
		<field>
			<name>c_L4</name>
			<definition>Maximum unprojected likelihood, c_L</definition>
			<units>---</units></field>
		<field>
			<name>phi_E4</name>
			<definition>Maximum unprojected likelihood, phi_E</definition>
			<units>---</units></field>
		<field>
			<name>theta_E4</name>
			<definition>Maximum unprojected likelihood, theta_E</definition>
			<units>---</units></field></fields></tableHead>
	
			<textFile xlink:href="table5.tex"><name>table5.tex</name><description><para>AASTeX version of table5.dat</para></description></textFile>
	<history>
		<ingest>
	
			<creator>
				<lastName>Lee Brotzman</lastName>
				<affiliation>ADS</affiliation></creator>
	<date>
		<year>1994</year><month>Oct</month><day>10</day></date><acknowledgement>Statler T.S.                          tss@physics.unc.edu
      Department of Physics and Astronomy, CB# 3255, University of North
       Carolina, Chapel Hill, North Carolina 25799-3255
   AAS CD-ROM series, Volume 3, 1995</acknowledgement></ingest>
		</history>
	<identifier>J_AJ_108_111.xml</identifier></dataset>
