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<item>
            <title>[PIPE2D-642] Stellar typing with SDSS broad-band data</title>
                <link>https://pfspipe.ipmu.jp/jira/browse/PIPE2D-642</link>
                <project id="10002" key="PIPE2D">DRP 2-D Pipeline</project>
                    <description>&lt;p&gt;Classify stellar types of HSC stellar objects with HSC broad band data and find the best fit template using SDSS photometries. Test a case without u-band.&lt;/p&gt;</description>
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        <key id="14922">PIPE2D-642</key>
            <summary>Stellar typing with SDSS broad-band data</summary>
                <type id="10001" iconUrl="https://pfspipe.ipmu.jp/jira/secure/viewavatar?size=xsmall&amp;avatarId=10515&amp;avatarType=issuetype">Story</type>
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                    <statusCategory id="3" key="done" colorName="green"/>
                                    <resolution id="10000">Done</resolution>
                                        <assignee username="takuji.yamashita">Takuji Yamashita</assignee>
                                    <reporter username="takuji.yamashita">Takuji Yamashita</reporter>
                        <labels>
                            <label>flux-calibration</label>
                    </labels>
                <created>Fri, 9 Oct 2020 05:21:53 +0000</created>
                <updated>Mon, 4 Jan 2021 20:23:22 +0000</updated>
                            <resolved>Mon, 12 Oct 2020 23:57:00 +0000</resolved>
                                                                        <due></due>
                            <votes>0</votes>
                                    <watches>2</watches>
                                                                <comments>
                            <comment id="17859" author="takuji.yamashita" created="Fri, 9 Oct 2020 05:53:46 +0000"  >&lt;p&gt;The results of SDSS broad band stellar typing. I use 22 stars in Lee et al. (2011) which have no problems in SDSS photometry and meet the crude color selection criteria for F stars defined in &lt;a href=&quot;https://pfspipe.ipmu.jp/jira/browse/PIPE2D-383&quot; title=&quot;Define crude criteria to select F-stars from HSC photometry&quot; class=&quot;issue-link&quot; data-issue-key=&quot;PIPE2D-383&quot;&gt;&lt;del&gt;PIPE2D-383&lt;/del&gt;&lt;/a&gt;. I test two cases: use the full filter set of ugriz and use only griz without u-band, to see an&#160;effectiveness of u-band in SED fitting.&lt;/p&gt;

&lt;p&gt;This figure is the robust RMS of fractional residuals between an SDSS spectrum and the best fit template. The left panel is the case of the full filter set, while the right is one without u-band. The difference is not big. The mean RMSs are 3.6% and 3.9% for the full filter set and for griz, respectively.&#160;&lt;/p&gt;

&lt;p&gt;&lt;span class=&quot;image-wrap&quot; style=&quot;&quot;&gt;&lt;a id=&quot;13112_thumb&quot; href=&quot;https://pfspipe.ipmu.jp/jira/secure/attachment/13112/13112_gr_sigmaclipRMS_wwou_v3.png&quot; title=&quot;gr_sigmaclipRMS_wwou_v3.png&quot; file-preview-type=&quot;image&quot; file-preview-id=&quot;13112&quot; file-preview-title=&quot;gr_sigmaclipRMS_wwou_v3.png&quot;&gt;&lt;img src=&quot;https://pfspipe.ipmu.jp/jira/secure/thumbnail/13112/_thumb_13112.png&quot; height=&quot;274&quot; width=&quot;559&quot; style=&quot;border: 0px solid black&quot; /&gt;&lt;/a&gt;&lt;/span&gt;&lt;/p&gt;

&lt;p&gt;&#160;&lt;/p&gt;</comment>
                            <comment id="17860" author="takuji.yamashita" created="Fri, 9 Oct 2020 06:01:46 +0000"  >&lt;p&gt;The SDSS - AB mag offset was corrected using the offset derived by David Hogg (&lt;a href=&quot;https://arxiv.org/abs/1711.01122&quot; class=&quot;external-link&quot; rel=&quot;nofollow&quot;&gt;https://arxiv.org/abs/1711.01122&lt;/a&gt;).&lt;/p&gt;</comment>
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            <issuekey id="14302">PIPE2D-538</issuekey>
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                            <attachment id="13112" name="gr_sigmaclipRMS_wwou_v3.png" size="29677" author="takuji.yamashita" created="Fri, 9 Oct 2020 05:49:40 +0000"/>
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