Figure Sets

Capture figure sets using a <fig-group> element.

<fig-group> elements must not be captured as a child of  they must instead be a direct child of the parent structure (usually a <sec> or <body> element).

Each <fig-group> must have the following attributes:


Attribute Name	Attribute Value
id	[FigID]
content-type	figureset
position	float

Each <fig-group> element must have a <caption> child element. The <caption> element must contain:

A <title> element
The text of the caption in one or more  elements.
The linking text that appears in the print version in a  element with a @content-type attribute of value print.
The linking text that appears in the online version in a  element with a @content-type attribute of value online.
The figure set title in a  element with a @content-type attribute of value figureset.
The description of the figure set parts in a  element with a @content-type attribute of value numparts.

Optionally an <inline-supplementary-material> may be used as a child of caption to capture the file name of the tar of the figure set (see Inline Supplementary Data)

Each <fig-group> element must contain at least two child <fig> elements. These <fig> elements must follow the standard instructions found here: Figures with the exception that <label> and <caption> child elements are mandatory.

The <caption> element of each individual <fig> in the figure set must have two child  elements. One containing the figsetgrptitle and one containing the figsetgrpnote from the TeX input.

Example

<fig-group content-type="figureset" id="apjac5970f1" position="float">
  <caption>
    <title>Figure 1.</title>
    <p>Analysis of the stacked RC for Bin 5 of the spiral galaxy sample by
    Persic et al. (<xref ref-type="bibr" rid="apjac5970bib85">1996</xref>). The top left panel illustrate the RC curve data (open
    symbols) and the best-fit model for the Burkert (cyan line), NFW
    (orange line), and NMC profile (red line). The outcome of the Bayesian
    Markov Chain Monte Carlo parameter estimations are shown as corner
    plots for the Burkert profile (top-right panel), for the NFW profile
    (bottom left), and for the NMC model (bottom right, with purple
    contours representing the posterior when the halo concentration is
    constrained by the relation of Dutton &amp; Macciò <xref ref-type="bibr" rid="apjac5970bib36">2014</xref>, given by Equation
    (<xref ref-type="disp-formula" rid="apjac5970eqn18">18</xref>)).</p>
    <p content-type="print">(The complete figure set (11 images) is available
    in the <ext-link xlink:href="https://doi.org/10.3847/1538-4357/ac5970">online article</ext-link>.)</p>
    <p content-type="online">(The <inline-supplementary-material content-type="Tar file" xlink:title="Tarball of figure set images" xlink:href="apjac5970figset1.tar.gz">complete figure
  set</inline-supplementary-material> (11 images) is available.)</p>
<p content-type="figureset">Analysis of the stacked RCs for the spiral
  galaxy sample by Persic et al. (1996).</p>
    <p content-type="numparts">Figure 1.1–1.11 (1 of 11 images)</p>
  </caption>
  <fig fig-type="print" id="apjac5970f1_pr" position="float">
    <graphic content-type="print" id="apjac5970f1_eps" xlink:href="apjac5970f1.eps"/>
    <graphic content-type="online" id="apjac5970f1_lr" xlink:href="apjac5970f1_lr.jpg"/>
    <graphic content-type="high" id="apjac5970f1_hr" xlink:href="apjac5970f1_hr.jpg"/>
  </fig>
  <fig fig-type="online" id="apjac5970f1_1" position="float">
    <label>Figure 1.1.</label>
    <caption>
      <p>Bin 1 of PSS96</p>
      <p>Analysis of the stacked RC of the spiral galaxy sample by Persic et
    al. (1996). The top left panel illustrate the RC curve data (open
    symbols) and the best-fit model for the Burkert (cyan line), NFW
    (orange line) and NMC profile (red line). The outcome of the
    Bayesian MCMC parameter estimation are shown as corner plots for
    the Burkert profile (top right panel), for the NFW profile (bottom
    left) and for the NMC model (bottom right, with purple contours
    representing the posterior when the halo concentration is
    constrained by the relation of Dutton &amp; Macciò (2014) given by
    Equation (18)).</p>
    </caption>
    <graphic content-type="online" id="apjac5970f1_1_lr" xlink:href="apjac5970f1_1_lr.jpg"/>
    <graphic content-type="high" id="apjac5970f1_1_hr" xlink:href="apjac5970f1_1_hr.jpg"/>
  </fig>
  <fig fig-type="online" id="apjac5970f1_2" position="float">
    <label>Figure 1.2.</label>
    <caption>
      <p>Bin 2 of PSS96</p>
      <p>Analysis of the stacked RC of the spiral galaxy sample by Persic et
    al. (1996). The top left panel illustrate the RC curve data (open
    symbols) and the best-fit model for the Burkert (cyan line), NFW
    (orange line) and NMC profile (red line). The outcome of the
    Bayesian MCMC parameter estimation are shown as corner plots for
    the Burkert profile (top right panel), for the NFW profile (bottom
    left) and for the NMC model (bottom right, with purple contours
    representing the posterior when the halo concentration is
    constrained by the relation of Dutton &amp; Macciò (2014) given by
    Equation (18)).</p>
    </caption>
    <graphic content-type="online" id="apjac5970f1_2_lr" xlink:href="apjac5970f1_2_lr.jpg"/>
    <graphic content-type="high" id="apjac5970f1_2_hr" xlink:href="apjac5970f1_2_hr.jpg"/>
  </fig>
  <fig fig-type="online" id="apjac5970f1_3" position="float">
    <label>Figure 1.3.</label>
    <caption>
      <p>Bin 3 of PSS96</p>
      <p>Analysis of the stacked RC of the spiral galaxy sample by Persic et
    al. (1996). The top left panel illustrate the RC curve data (open
    symbols) and the best-fit model for the Burkert (cyan line), NFW
    (orange line) and NMC profile (red line). The outcome of the
    Bayesian MCMC parameter estimation are shown as corner plots for
    the Burkert profile (top right panel), for the NFW profile (bottom
    left) and for the NMC model (bottom right, with purple contours
    representing the posterior when the halo concentration is
    constrained by the relation of Dutton &amp; Macciò (2014) given by
    Equation (18)).</p>
    </caption>
    <graphic content-type="online" id="apjac5970f1_3_lr" xlink:href="apjac5970f1_3_lr.jpg"/>
    <graphic content-type="high" id="apjac5970f1_3_hr" xlink:href="apjac5970f1_3_hr.jpg"/>
  </fig>
  <fig fig-type="online" id="apjac5970f1_4" position="float">
    <label>Figure 1.4.</label>
    <caption>
      <p>Bin 4 of PSS96</p>
      <p>Analysis of the stacked RC of the spiral galaxy sample by Persic et
    al. (1996). The top left panel illustrate the RC curve data (open
    symbols) and the best-fit model for the Burkert (cyan line), NFW
    (orange line) and NMC profile (red line). The outcome of the
    Bayesian MCMC parameter estimation are shown as corner plots for
    the Burkert profile (top right panel), for the NFW profile (bottom
    left) and for the NMC model (bottom right, with purple contours
    representing the posterior when the halo concentration is
    constrained by the relation of Dutton &amp; Macciò (2014) given by
    Equation (18)).</p>
    </caption>
    <graphic content-type="online" id="apjac5970f1_4_lr" xlink:href="apjac5970f1_4_lr.jpg"/>
    <graphic content-type="high" id="apjac5970f1_4_hr" xlink:href="apjac5970f1_4_hr.jpg"/>
  </fig>
  <fig fig-type="online" id="apjac5970f1_5" position="float">
    <label>Figure 1.5.</label>
    <caption>
      <p>Bin 5 of PSS96</p>
      <p>Analysis of the stacked RC of the spiral galaxy sample by Persic et
    al. (1996). The top left panel illustrate the RC curve data (open
    symbols) and the best-fit model for the Burkert (cyan line), NFW
    (orange line) and NMC profile (red line). The outcome of the
    Bayesian MCMC parameter estimation are shown as corner plots for
    the Burkert profile (top right panel), for the NFW profile (bottom
    left) and for the NMC model (bottom right, with purple contours
    representing the posterior when the halo concentration is
    constrained by the relation of Dutton &amp; Macciò (2014) given by
    Equation (18)).</p>
    </caption>
    <graphic content-type="online" id="apjac5970f1_5_lr" xlink:href="apjac5970f1_5_lr.jpg"/>
    <graphic content-type="high" id="apjac5970f1_5_hr" xlink:href="apjac5970f1_5_hr.jpg"/>
  </fig>
  <fig fig-type="online" id="apjac5970f1_6" position="float">
    <label>Figure 1.6.</label>
    <caption>
      <p>Bin 6 of PSS96</p>
      <p>Analysis of the stacked RC of the spiral galaxy sample by Persic et
    al. (1996). The top left panel illustrate the RC curve data (open
    symbols) and the best-fit model for the Burkert (cyan line), NFW
    (orange line) and NMC profile (red line). The outcome of the
    Bayesian MCMC parameter estimation are shown as corner plots for
    the Burkert profile (top right panel), for the NFW profile (bottom
    left) and for the NMC model (bottom right, with purple contours
    representing the posterior when the halo concentration is
    constrained by the relation of Dutton &amp; Macciò (2014) given by
    Equation (18)).</p>
    </caption>
    <graphic content-type="online" id="apjac5970f1_6_lr" xlink:href="apjac5970f1_6_lr.jpg"/>
    <graphic content-type="high" id="apjac5970f1_6_hr" xlink:href="apjac5970f1_6_hr.jpg"/>
  </fig>
  <fig fig-type="online" id="apjac5970f1_7" position="float">
    <label>Figure 1.7.</label>
    <caption>
      <p>Bin 7 of PSS96</p>
      <p>Analysis of the stacked RC of the spiral galaxy sample by Persic et
    al. (1996). The top left panel illustrate the RC curve data (open
    symbols) and the best-fit model for the Burkert (cyan line), NFW
    (orange line) and NMC profile (red line). The outcome of the
    Bayesian MCMC parameter estimation are shown as corner plots for
    the Burkert profile (top right panel), for the NFW profile (bottom
    left) and for the NMC model (bottom right, with purple contours
    representing the posterior when the halo concentration is
    constrained by the relation of Dutton &amp; Macciò (2014) given by
    Equation (18)).</p>
    </caption>
    <graphic content-type="online" id="apjac5970f1_7_lr" xlink:href="apjac5970f1_7_lr.jpg"/>
    <graphic content-type="high" id="apjac5970f1_7_hr" xlink:href="apjac5970f1_7_hr.jpg"/>
  </fig>
  <fig fig-type="online" id="apjac5970f1_8" position="float">
    <label>Figure 1.8.</label>
    <caption>
      <p>Bin 8 of PSS96</p>
      <p>Analysis of the stacked RC of the spiral galaxy sample by Persic et
    al. (1996). The top left panel illustrate the RC curve data (open
    symbols) and the best-fit model for the Burkert (cyan line), NFW
    (orange line) and NMC profile (red line). The outcome of the
    Bayesian MCMC parameter estimation are shown as corner plots for
    the Burkert profile (top right panel), for the NFW profile (bottom
    left) and for the NMC model (bottom right, with purple contours
    representing the posterior when the halo concentration is
    constrained by the relation of Dutton &amp; Macciò (2014) given by
    Equation (18)).</p>
    </caption>
    <graphic content-type="online" id="apjac5970f1_8_lr" xlink:href="apjac5970f1_8_lr.jpg"/>
    <graphic content-type="high" id="apjac5970f1_8_hr" xlink:href="apjac5970f1_8_hr.jpg"/>
  </fig>
  <fig fig-type="online" id="apjac5970f1_9" position="float">
    <label>Figure 1.9.</label>
    <caption>
      <p>Bin 9 of PSS96</p>
      <p>Analysis of the stacked RC of the spiral galaxy sample by Persic et
    al. (1996). The top left panel illustrate the RC curve data (open
    symbols) and the best-fit model for the Burkert (cyan line), NFW
    (orange line) and NMC profile (red line). The outcome of the
    Bayesian MCMC parameter estimation are shown as corner plots for
    the Burkert profile (top right panel), for the NFW profile (bottom
    left) and for the NMC model (bottom right, with purple contours
    representing the posterior when the halo concentration is
    constrained by the relation of Dutton &amp; Macciò (2014) given by
    Equation (18)).</p>
    </caption>
    <graphic content-type="online" id="apjac5970f1_9_lr" xlink:href="apjac5970f1_9_lr.jpg"/>
    <graphic content-type="high" id="apjac5970f1_9_hr" xlink:href="apjac5970f1_9_hr.jpg"/>
  </fig>
  <fig fig-type="online" id="apjac5970f1_10" position="float">
    <label>Figure 1.10.</label>
    <caption>
      <p>Bin 10 of PSS96</p>
      <p>Analysis of the stacked RC of the spiral galaxy sample by Persic et
    al. (1996). The top left panel illustrate the RC curve data (open
    symbols) and the best-fit model for the Burkert (cyan line), NFW
    (orange line) and NMC profile (red line). The outcome of the
    Bayesian MCMC parameter estimation are shown as corner plots for
    the Burkert profile (top right panel), for the NFW profile (bottom
    left) and for the NMC model (bottom right, with purple contours
    representing the posterior when the halo concentration is
    constrained by the relation of Dutton &amp; Macciò (2014) given by
    Equation (18)).</p>
    </caption>
    <graphic content-type="online" id="apjac5970f1_10_lr" xlink:href="apjac5970f1_10_lr.jpg"/>
    <graphic content-type="high" id="apjac5970f1_10_hr" xlink:href="apjac5970f1_10_hr.jpg"/>
  </fig>
  <fig fig-type="online" id="apjac5970f1_11" position="float">
    <label>Figure 1.11.</label>
    <caption>
      <p>Bin 11 of PSS96</p>
      <p>Analysis of the stacked RC of the spiral galaxy sample by Persic et
    al. (1996). The top left panel illustrate the RC curve data (open
    symbols) and the best-fit model for the Burkert (cyan line), NFW
    (orange line) and NMC profile (red line). The outcome of the
    Bayesian MCMC parameter estimation are shown as corner plots for
    the Burkert profile (top right panel), for the NFW profile (bottom
    left) and for the NMC model (bottom right, with purple contours
    representing the posterior when the halo concentration is
    constrained by the relation of Dutton &amp; Macciò (2014) given by
    Equation (18)).</p>
    </caption>
    <graphic content-type="online" id="apjac5970f1_11_lr" xlink:href="apjac5970f1_11_lr.jpg"/>
    <graphic content-type="high" id="apjac5970f1_11_hr" xlink:href="apjac5970f1_11_hr.jpg"/>
  </fig>
</fig-group>