January 31, 2022 Dataset Open Access

Boschini, M.J.; Della Torre, S.; Gervasi, M.; La Vacca, G.; Rancoita, P.G.

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  <identifier identifierType="DOI">10.15161/oar.it/75359</identifier>
  <creators>
    <creator>
      <creatorName>Boschini, M.J.</creatorName>
      <givenName>M.J.</givenName>
      <familyName>Boschini</familyName>
      <nameIdentifier nameIdentifierScheme="ORCID" schemeURI="http://orcid.org/">0000-0002-6401-0457</nameIdentifier>
      <affiliation>CINECA, Segrate, Milano, Italy</affiliation>
    </creator>
    <creator>
      <creatorName>Della Torre, S.</creatorName>
      <givenName>S.</givenName>
      <familyName>Della Torre</familyName>
      <nameIdentifier nameIdentifierScheme="ORCID" schemeURI="http://orcid.org/">0000-0002-7669-0859</nameIdentifier>
      <affiliation>INFN, Milano-Bicocca, Milano, Italy</affiliation>
    </creator>
    <creator>
      <creatorName>Gervasi, M.</creatorName>
      <givenName>M.</givenName>
      <familyName>Gervasi</familyName>
      <nameIdentifier nameIdentifierScheme="ORCID" schemeURI="http://orcid.org/">0000-0003-3884-0905</nameIdentifier>
      <affiliation>Physics Department, University of Milano-Bicocca, Milano, Italy</affiliation>
    </creator>
    <creator>
      <creatorName>La Vacca, G.</creatorName>
      <givenName>G.</givenName>
      <familyName>La Vacca</familyName>
      <nameIdentifier nameIdentifierScheme="ORCID" schemeURI="http://orcid.org/">0000-0002-2168-9447</nameIdentifier>
      <affiliation>Physics Department, University of Milano-Bicocca, Piazza della Scienza, 3, 20126 Milano, Italy</affiliation>
    </creator>
    <creator>
      <creatorName>Rancoita, P.G.</creatorName>
      <givenName>P.G.</givenName>
      <familyName>Rancoita</familyName>
      <nameIdentifier nameIdentifierScheme="ORCID" schemeURI="http://orcid.org/">0000-0002-1990-4283</nameIdentifier>
      <affiliation>INFN sez. Milano-Bicocca, Piazza della Scienza, 3, 20126 Milano, Italy</affiliation>
    </creator>
  </creators>
  <titles>
    <title>Modulation Module for HelMod-4</title>
  </titles>
  <publisher>INFN Open Access Repository</publisher>
  <publicationYear>2022</publicationYear>
  <subjects>
    <subject>solar modulation</subject>
    <subject>cosmic rays</subject>
    <subject>particle propagation</subject>
  </subjects>
  <dates>
    <date dateType="Issued">2022-01-31</date>
  </dates>
  <language>en</language>
  <resourceType resourceTypeGeneral="Dataset"/>
  <alternateIdentifiers>
    <alternateIdentifier alternateIdentifierType="url">https://www.openaccessrepository.it/record/75359</alternateIdentifier>
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  <relatedIdentifiers>
    <relatedIdentifier relatedIdentifierType="DOI" relationType="IsReferencedBy">10.1002/2015JA022237</relatedIdentifier>
    <relatedIdentifier relatedIdentifierType="DOI" relationType="IsReferencedBy">10.1016/j.asr.2019.04.007</relatedIdentifier>
    <relatedIdentifier relatedIdentifierType="URL" relationType="IsDocumentedBy">https://www.helmod.org</relatedIdentifier>
    <relatedIdentifier relatedIdentifierType="DOI" relationType="IsVersionOf">10.15161/oar.it/75358</relatedIdentifier>
    <relatedIdentifier relatedIdentifierType="URL" relationType="IsPartOf">https://www.openaccessrepository.it/communities/infn</relatedIdentifier>
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  <version>4.3</version>
  <rightsList>
    <rights rightsURI="https://creativecommons.org/licenses/by/4.0/">Creative Commons Attribution 4.0</rights>
    <rights rightsURI="info:eu-repo/semantics/openAccess">Open Access</rights>
  </rightsList>
  <descriptions>
    <description descriptionType="Abstract">&lt;p&gt;The SDE integration with HelMod results in a quite expensive effort from the computational point of view since,&amp;nbsp;to minimize the uncertainties, a huge amount of events should be integrated from Earth to the heliosphere boundary.&amp;nbsp;Monte Carlo integration allows us to evaluate the normalized probability function (G) that a particle observed at Earth with rigidity R0 entered into the heliosphere with rigidity R. The convolution of the normalized probability function with the very local interstellar spectra result in the modulation of differential intensity for the time and solar distance where G was evaluated. In the present dataset, we provide the numerical output of&amp;nbsp;HelMod-4 model (www.helmod.org) in the form of&amp;nbsp;normalized probability histograms. The python script attached is able to convert GALPROP output (or plain text LIS file) to modulated spectrum for periods of selected experiments.&lt;/p&gt;

&lt;p&gt;This dataset was used as part of the publications in the references.&lt;/p&gt;

&lt;p&gt;For any information about the HelMod-4 Model, please refer to the official &lt;a href="http://www.helmod.org"&gt;website&lt;/a&gt;.&lt;/p&gt;

&lt;p&gt;&lt;strong&gt;How to install and configure&amp;nbsp;&lt;/strong&gt;&lt;/p&gt;

&lt;p&gt;Install python (&amp;gt;3.0) packages&lt;/p&gt;

&lt;ul&gt;
	&lt;li&gt;&lt;a href="https://www.astropy.org/"&gt;astropy&lt;/a&gt;&lt;/li&gt;
	&lt;li&gt;&lt;a href="https://www.scipy.org/"&gt;scypy&lt;/a&gt; &amp;gt;=0.17.0&lt;/li&gt;
	&lt;li&gt;&lt;a href="https://numpy.org/"&gt;numpy&lt;/a&gt; &amp;gt;=1.10&lt;/li&gt;
	&lt;li&gt;&lt;a href="https://matplotlib.org/"&gt;matplotlib&lt;/a&gt;&lt;/li&gt;
&lt;/ul&gt;

&lt;p&gt;Download the&amp;nbsp;Python OfflineModule and the HelModArchive. The archive is provided in tgz format, thus it needs to be first unpacked with the command &lt;code&gt;tar -xvzf &amp;lt;ArchiveName&amp;gt;.tgz&lt;/code&gt;.&amp;nbsp;&lt;/p&gt;

&lt;p&gt;The archive&amp;nbsp;structure:&lt;/p&gt;

&lt;p&gt;The HelModArchives.tgz contains several directories each one with the name of a space or balloon mission. Each folder should be considered as an&amp;nbsp;HelMod Archive containing the following files:&lt;/p&gt;

&lt;ul&gt;
	&lt;li&gt;&lt;em&gt;ExpList.list &lt;/em&gt;: List of nuclei and isotopes simulated (to not modify)&lt;/li&gt;
	&lt;li&gt;&lt;em&gt;ExpList_Plot.list&lt;/em&gt;:&amp;nbsp;List of nuclei available in the archive, reference and plots properties (do not modify first and second columns, the others can be updated to modify the output plots)&lt;/li&gt;
	&lt;li&gt;&lt;em&gt;ParameterSimulated.list&lt;/em&gt;: list of folders in the form RawPar_HelMod4_XX,&amp;nbsp; (&lt;em&gt;at least one line should start with &amp;#39;+&amp;#39;, if not, please add it to first line&lt;/em&gt;)&lt;/li&gt;
	&lt;li&gt;&lt;em&gt;ParameterSimulated_DB.list&lt;/em&gt;:&amp;nbsp;list of folders in the form RawPar_HelMod4_XX, with description&lt;/li&gt;
	&lt;li&gt;&lt;em&gt;Version.txt &lt;/em&gt;: Version notes&lt;/li&gt;
	&lt;li&gt;&lt;em&gt;DataTXT&lt;/em&gt; : experimental energy and rigidity binning used for simulations&lt;/li&gt;
	&lt;li&gt;&lt;em&gt;RawPar_HelMod4_00&lt;/em&gt; : HelMod simulations outputs&lt;/li&gt;
&lt;/ul&gt;

&lt;p&gt;&lt;strong&gt;How to use the module&lt;/strong&gt;:&lt;/p&gt;

&lt;p&gt;The usage of the module requires three elements:&lt;/p&gt;

&lt;ul&gt;
	&lt;li&gt;An Helmod Archive unpacked in some known folder. E.g. let&amp;#39;s &amp;lt;ArcPath&amp;gt;=/home/test/Archive1&lt;/li&gt;
	&lt;li&gt;A &lt;a href="http://www.helmod.org/index.php/local-interstellar-spectra"&gt;LIS&lt;/a&gt; from galprop fits file OR plain text file format (hereafter called &lt;code&gt;&amp;lt;LIS_FILE&amp;gt;&lt;/code&gt;).&amp;nbsp;&lt;/li&gt;
	&lt;li&gt;The label of the ion/dataset (hereafter called &lt;code&gt;&amp;lt;ExpNameKey&amp;gt;&lt;/code&gt;) that are intended to be modulated.&lt;/li&gt;
&lt;/ul&gt;

&lt;p&gt;The list of available&amp;nbsp;&lt;code&gt;&amp;lt;ExpNameKey&amp;gt;&lt;/code&gt;&amp;nbsp; in each archive may be found in the file&amp;nbsp;ExpList_Plot.list&amp;nbsp;or using the command-line&amp;nbsp;&lt;/p&gt;

&lt;pre&gt;&lt;code class="language-bash"&gt;python3 HelMod_Module.py -a &amp;lt;ArcPath&amp;gt; -l&lt;/code&gt;&lt;/pre&gt;

&lt;p&gt;The basic command to get the modulated spectrum is:&lt;/p&gt;

&lt;pre&gt;&lt;code class="language-bash"&gt;python3 HelMod_Module.py -a &amp;lt;ArcPath&amp;gt; --LIS &amp;lt;LIS_FILE&amp;gt; --SimName &amp;lt;ExpNameKey&amp;gt;&lt;/code&gt;&lt;/pre&gt;

&lt;p&gt;other available options:&lt;/p&gt;

&lt;ul&gt;
	&lt;li&gt;&lt;code&gt;&lt;em&gt;-h&lt;/em&gt;&amp;nbsp;&lt;/code&gt;help description&lt;/li&gt;
	&lt;li&gt;&lt;em&gt;&lt;code&gt;-t&lt;/code&gt;&lt;/em&gt;&amp;nbsp;use this option to specify that &amp;lt;LIS_FILE&amp;gt; is a two-column plain text file (see below).&lt;/li&gt;
	&lt;li&gt;&lt;code&gt;&lt;em&gt;-p &amp;lt;PAR_SET_NAME&amp;gt;&lt;/em&gt;&amp;nbsp;&amp;nbsp;&lt;/code&gt;Choose a different set of parameters. The list of available parameter set names is available in the file &lt;em&gt;ParameterSimulated_DB.list .&lt;/em&gt;&lt;/li&gt;
	&lt;li&gt;&lt;em&gt;&lt;code&gt;--MakePlot&lt;/code&gt;Create&lt;/em&gt; a Plot in png format.&lt;/li&gt;
	&lt;li&gt;&lt;code&gt;&lt;em&gt;--SumAllIsotpes&lt;/em&gt;&amp;nbsp;&lt;/code&gt;(can be used with GALPROP LIS inputs) evaluate the modulated spectra as the sum of the modulated isotopes spectra (note that without this option only the LIS of the isotope specified in &amp;lt;ExpNameKey&amp;gt;&amp;nbsp;is considered by the script).&amp;nbsp;&lt;/li&gt;
	&lt;li&gt;&lt;code&gt;&lt;em&gt;--PrintLIS&lt;/em&gt;&amp;nbsp; &lt;/code&gt;Create a file with the&amp;nbsp;LIS in the format of a two-column plain text file.&lt;/li&gt;
	&lt;li&gt;&lt;code&gt;&lt;em&gt;--SimUnit &amp;lt;Tkin/Rigi&amp;gt;&lt;/em&gt;&amp;nbsp;&lt;/code&gt;force the Output Unit of the module: use &lt;em&gt;Tkin&lt;/em&gt; to select&amp;nbsp;Kinetic Energy per Nucleon [GeV/n], use&amp;nbsp;&lt;em&gt;Rigi&lt;/em&gt;&amp;nbsp;to select Rigidity [GV].&amp;nbsp;If not specified,&amp;nbsp;the output is chosen accordingly to the original format of the experimental dataset.&lt;/li&gt;
	&lt;li&gt;&lt;em&gt;&lt;code&gt;-&lt;/code&gt;&lt;/em&gt;&lt;code&gt;&lt;em&gt;o &amp;lt;FILE_NAME&amp;gt;&lt;/em&gt;&amp;nbsp;&lt;/code&gt;Use a custom name for the output file.&lt;/li&gt;
&lt;/ul&gt;

&lt;p&gt;&lt;strong&gt;LIS in text format&lt;/strong&gt;&lt;/p&gt;

&lt;p&gt;Users can provide a txt file for LIS with the following characteristics:&lt;/p&gt;

&lt;ul&gt;
	&lt;li&gt;The file must be a text file.&lt;/li&gt;
	&lt;li&gt;The file must contain two columns only:
	&lt;ol&gt;
		&lt;li&gt;one for kinetic energy per nucleon [GeV]&lt;/li&gt;
		&lt;li&gt;the second for the LIS flux [ (m&lt;sup&gt;2&lt;/sup&gt;&amp;nbsp;s sr GeV)&lt;sup&gt;-1&lt;/sup&gt;].&lt;/li&gt;
	&lt;/ol&gt;
	&lt;/li&gt;
	&lt;li&gt;The file may contain&amp;nbsp;comments. Line starting with &amp;#39;#&amp;#39; character will be ignored.&lt;/li&gt;
&lt;/ul&gt;</description>
    <description descriptionType="Other">{"references": ["Boschini et al (2022) Astrophys. J. 925(2):108 http://dx.doi.org/10.3847/1538-4357/ac313d", "Boschini et al (2021) Astrophys. J. 913(1):5 http://dx.doi.org/10.3847/1538-4357/abf11c", "Boschini et al (2020) Astrophys. J. Supplement 250(2):27 http://dx.doi.org/10.3847/1538-4365/aba901", "Boschini et al (2020) Astrophys. J. 889(2):167, 2020. http://dx.doi.org/10.3847/1538-4357/ab64f1", "Boschini et al (2019) Advances in Space Research 64(12):2459 - 2476 http://dx.doi.org/10.1016/j.asr.2019.04.007"]}</description>
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