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notebooks/IFU_cube_continuum_fit/NGC4151_FeII_ContinuumFit.html

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 <h3>Alternative way to do continuum subtraction using numpy<a class="headerlink" href="#alternative-way-to-do-continuum-subtraction-using-numpy" title="Permalink to this heading">#</a></h3>

notebooks/MRS_Mstar_analysis/JWST_Mstar_dataAnalysis_analysis.html

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 <section id="load-in-the-spectrum-list-from-above-note-only-the-first-spectrum-in-your-list-is-displayed-automatically-you-will-need-to-turn-on-the-remaining-spectra-in-the-data-drop-down-then-hit-the-home-button-in-the-toolbar-and-scale-our-plot-accordingly-to-see-the-other-spectra">
 <h4>Load in the spectrum list from above. Note, only the first spectrum in your list is displayed automatically. You will need to turn on the remaining spectra in the “DATA” drop-down, then hit the “Home” button in the toolbar, and scale our plot accordingly to see the other spectra.<a class="headerlink" href="#load-in-the-spectrum-list-from-above-note-only-the-first-spectrum-in-your-list-is-displayed-automatically-you-will-need-to-turn-on-the-remaining-spectra-in-the-data-drop-down-then-hit-the-home-button-in-the-toolbar-and-scale-our-plot-accordingly-to-see-the-other-spectra" title="Permalink to this heading">#</a></h4>
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 <section id="developer-note-need-to-pick-a-different-unit-than-meters-https-jira-stsci-edu-browse-jdat-1792">
 <h3>Developer Note. Need to pick a different unit than meters. https://jira.stsci.edu/browse/JDAT-1792<a class="headerlink" href="#developer-note-need-to-pick-a-different-unit-than-meters-https-jira-stsci-edu-browse-jdat-1792" title="Permalink to this heading">#</a></h3>
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 <h3>Developer Note: Cannot currently open a spectrum1d output from cubeviz in specviz.  https://jira.stsci.edu/browse/JDAT-1791<a class="headerlink" href="#developer-note-cannot-currently-open-a-spectrum1d-output-from-cubeviz-in-specviz-https-jira-stsci-edu-browse-jdat-1791" title="Permalink to this heading">#</a></h3>
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notebooks/NIRISS/NIRISS_WFSS_advanced/01_niriss_wfss_image2_image3.html

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 <p>The segmentation maps are also a product of the Image3 pipeline, and they are used the help determine the source catalog. Let’s take a look at those to ensure we are happy with what it is defining as a source.</p>
 <p>In the segmentation map, each blue blob should correspond to a physical target. There are cases where sources can be blended, in which case the parameters for making the semgentation map and source catalog should be changed. An example of this can be seen below in the observation 004 F200W filter image where two galaxies at ~(1600, 1300) have been blended into one source. This is discussed in more detail below in <span class="xref myst">Custom Imaging Pipeline Run</span>.</p>
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   exp_obj = getattr(self._obj, attr)
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 <p>The cell below shows similar information using Imviz instead to visualize this.</p>
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 <a class="reference internal image-reference" href="https://raw.githubusercontent.com/spacetelescope/notebooks/master/assets/stsci_pri_combo_mark_horizonal_white_bkgd.png"><img alt="Space Telescope Logo" src="https://raw.githubusercontent.com/spacetelescope/notebooks/master/assets/stsci_pri_combo_mark_horizonal_white_bkgd.png" style="width: 200px;" /></a>
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notebooks/NIRISS/niriss_imaging/niriss-imaging-tutorial.html

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notebooks/NIRISS_WFSS_advanced/01_niriss_wfss_image2_image3.html

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 <p>The segmentation maps are also a product of the Image3 pipeline, and they are used the help determine the source catalog. Let’s take a look at those to ensure we are happy with what it is defining as a source.</p>
 <p>In the segmentation map, each blue blob should correspond to a physical target. There are cases where sources can be blended, in which case the parameters for making the semgentation map and source catalog should be changed. An example of this can be seen below in the observation 004 F200W filter image where two galaxies at ~(1600, 1300) have been blended into one source. This is discussed in more detail below in <span class="xref myst">Custom Imaging Pipeline Run</span>.</p>
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 <p>The cell below shows similar information using Imviz instead to visualize this.</p>
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 <div class="output stream highlight-myst-ansi notranslate"><div class="highlight"><pre><span></span>Plotting: default_image3_calibrated/jw02079-o004_t001_niriss_clear-f150w_i2d.fits
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 <a class="reference internal image-reference" href="https://raw.githubusercontent.com/spacetelescope/notebooks/master/assets/stsci_pri_combo_mark_horizonal_white_bkgd.png"><img alt="Space Telescope Logo" src="https://raw.githubusercontent.com/spacetelescope/notebooks/master/assets/stsci_pri_combo_mark_horizonal_white_bkgd.png" style="width: 200px;" /></a>
 </section>

notebooks/NIRISS_WFSS_advanced/02_niriss_wfss_spec2.html

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 <p>We can then take a look at the extracted spectrum in this box both in the cal file and the x1d file. In the extracted spectrum below you can see the [OII] and H<span class="math notranslate nohighlight">\(\beta\)</span> emission lines from the galaxy.</p>
 <p><em>Note: The upturned edge effects seen in the 1-D spectrum are due to interpolation at the edges of the extraction box for the current flux calibration. This is also part of an ongoing calibration effort.</em></p>
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 <p>Overplot these files on top of each other to compare. The two grisms will be different line styles to draw attention to any differences that could be due to the calibration, including contamination, and each blocking filter will be a different color.</p>
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 <p>Continue to explore further, including using the <a class="reference external" href="https://jwst-pipeline.readthedocs.io/en/latest/jwst/pipeline/calwebb_spec3.html">spec3 stage</a> of the pipeline!</p>
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