{"id":954,"date":"2019-11-21T15:49:58","date_gmt":"2019-11-21T15:49:58","guid":{"rendered":"http:\/\/www.astrobulletin.univ.kiev.ua\/?p=954"},"modified":"2020-01-29T10:10:09","modified_gmt":"2020-01-29T10:10:09","slug":"59_parnovsky","status":"publish","type":"post","link":"https:\/\/astrobulletin.knu.ua\/ua\/59_parnovsky\/","title":{"rendered":"59_Parnovsky"},"content":{"rendered":"<p><span style=\"font-size: 10pt;\"><strong>Bulletin of Taras Shevchenko National University of Kyiv. Astronomy, no. 59, p. 9<span lang=\"en-US\">-12<\/span> (2019)<\/strong><\/span><\/p>\n<p><span style=\"font-size: 18pt; color: #333399;\"><strong>STUDY OF THE THERMAL EMISSION IN THE RADIO CONTINUUM AT 1.4 GHZ IN SELECTED COMPACT GALAXIES WITH ACTIVE STAR FORMATION\u00a0<\/strong><\/span><\/p>\n<p><strong>S. Parnovsky, Dr.Sci., professor<br \/>\nI. Izotova, PhD <\/strong><\/p>\n<p><strong>Taras Shevchenko National University of Kyiv, Kyiv, Ukraine\u00a0 \u00a0<\/strong><\/p>\n<p><!--more--><br \/>\n<strong>Abstract<\/strong><\/p>\n<p style=\"text-align: justify;\">The fraction of thermal (free-free) emission in the radio continuum at the frequency of 1.4 GHz is derived in subsample of 92 compact star-forming galaxies (CSFGs). These galaxies with detected radio emission and selected with a more strong compactness criterion represent the subsample of a larger sample of 193 galaxies (Parnovsky, S., &amp; Izotova, I.: 2018, BTSNU, 57(1), 41). We use the 1.4 GHz fluxes from the FIRST (Becker R.H.,White R.L., &amp; Helfand D.J.: 1995, ApJ, 450, 559). The fluxes of the thermal component at 1.4 GHz are derived from the extinction- and aperture-corrected fluxes of the H\u03b2 emission line in the SDSS spectra following to (Caplan, J., &amp; Deharveng, L.: 1986, A&amp;A, 155, 297) and are compared with the total fluxes in radio continuum. As well as for a complete sample of 193 galaxies, the distribution of the fraction of thermal emission A in the radio continuum at 1.4 GHz in subsample of 92 CSFGs is similar to the log-normal one with a median value of about 15%. We find that the fraction of thermal emission at 1.4 GHz is lower for the older starbursts. However, the results of the statistical analysis of the dependence of A on various parameters have been changed. For the complete sample, correlations of A with the equivalent width EW(H\u03b2) of the H\u03b2 emission line and the g \u2013 r colour index are revealed. For the subsample of 92 galaxies, the statistical significance of the correlation A with the colour index becomes negligible, and it corresponds to a confidence level of 92% for dependence of A on the equivalent width EW(H\u03b2). The reasons for the differences in the properties of these samples are discussed.<\/p>\n<p><strong>Key words<br \/>\n<\/strong>Star-forming galaxies, continuum radio emission, thermal emission<\/p>\n<p><strong>References<\/strong><\/p>\n<p><a href=\"http:\/\/www.astrobulletin.knu.ua\/wp-content\/uploads\/file\/59\/4.pdf\">Full text PDF<\/a><\/p>\n<p>DOI:\u00a0<a href=\"https:\/\/doi.org\/10.17721\/BTSNUA.2019.59.09-12\">https:\/\/doi.org\/10.17721\/BTSNUA.2019.59.09-12<\/a><\/p>","protected":false},"excerpt":{"rendered":"<p>\u0412\u0438\u0431\u0430\u0447\u0442\u0435 \u0446\u0435\u0439 \u0442\u0435\u043a\u0441\u0442 \u0434\u043e\u0441\u0442\u0443\u043f\u043d\u0438\u0439 \u0442\u0456\u043b\u044c\u043a\u0438 \u0432 &ldquo;English&rdquo;.<\/p>\n","protected":false},"author":2,"featured_media":0,"comment_status":"closed","ping_status":"open","sticky":false,"template":"","format":"standard","meta":{"footnotes":""},"categories":[23],"tags":[],"class_list":["post-954","post","type-post","status-publish","format-standard","hentry","category-number_59"],"_links":{"self":[{"href":"https:\/\/astrobulletin.knu.ua\/ua\/wp-json\/wp\/v2\/posts\/954","targetHints":{"allow":["GET"]}}],"collection":[{"href":"https:\/\/astrobulletin.knu.ua\/ua\/wp-json\/wp\/v2\/posts"}],"about":[{"href":"https:\/\/astrobulletin.knu.ua\/ua\/wp-json\/wp\/v2\/types\/post"}],"author":[{"embeddable":true,"href":"https:\/\/astrobulletin.knu.ua\/ua\/wp-json\/wp\/v2\/users\/2"}],"replies":[{"embeddable":true,"href":"https:\/\/astrobulletin.knu.ua\/ua\/wp-json\/wp\/v2\/comments?post=954"}],"version-history":[{"count":7,"href":"https:\/\/astrobulletin.knu.ua\/ua\/wp-json\/wp\/v2\/posts\/954\/revisions"}],"predecessor-version":[{"id":1073,"href":"https:\/\/astrobulletin.knu.ua\/ua\/wp-json\/wp\/v2\/posts\/954\/revisions\/1073"}],"wp:attachment":[{"href":"https:\/\/astrobulletin.knu.ua\/ua\/wp-json\/wp\/v2\/media?parent=954"}],"wp:term":[{"taxonomy":"category","embeddable":true,"href":"https:\/\/astrobulletin.knu.ua\/ua\/wp-json\/wp\/v2\/categories?post=954"},{"taxonomy":"post_tag","embeddable":true,"href":"https:\/\/astrobulletin.knu.ua\/ua\/wp-json\/wp\/v2\/tags?post=954"}],"curies":[{"name":"wp","href":"https:\/\/api.w.org\/{rel}","templated":true}]}}