1 Ocak 2022 Dergi makalesi Açık Erişim

Agarwal, Aditi; Mihov, B.; Andruchow, I; Cellone, Sergio A.; Anupama, G. C.; Agrawal, V; Zola, S.; Ozdonmez, Aykut; Ege, Ergun

JSON-LD (schema.org)

{
  "@context": "https://schema.org/", 
  "@id": 256847, 
  "@type": "ScholarlyArticle", 
  "creator": [
    {
      "@type": "Person", 
      "affiliation": "Raman Res Inst, CV Raman Ave, Sadashivanagar 560080, Bengaluru, India", 
      "name": "Agarwal, Aditi"
    }, 
    {
      "@type": "Person", 
      "name": "Mihov, B."
    }, 
    {
      "@type": "Person", 
      "name": "Andruchow, I"
    }, 
    {
      "@type": "Person", 
      "name": "Cellone, Sergio A."
    }, 
    {
      "@type": "Person", 
      "affiliation": "Indian Inst Astrophys, Block 2, Bangalore 560034, Karnataka, India", 
      "name": "Anupama, G. C."
    }, 
    {
      "@type": "Person", 
      "affiliation": "RMZ Ecoworld, Bellandur, Bangalore 560103, Karnataka, India", 
      "name": "Agrawal, V"
    }, 
    {
      "@type": "Person", 
      "name": "Zola, S."
    }, 
    {
      "@type": "Person", 
      "affiliation": "Ataturk Univ, Fac Sci, Dept Astron & Space Sci, Erzurum, Turkey", 
      "name": "Ozdonmez, Aykut"
    }, 
    {
      "@type": "Person", 
      "affiliation": "Istanbul Univ, Fac Sci, Dept Astron & Space Sci, TR-34116 Istanbul, Turkey", 
      "name": "Ege, Ergun"
    }
  ], 
  "datePublished": "2022-01-01", 
  "description": "We study flux and spectral variability of the high energy peaked TeV blazar PG 1553 + 113 on diverse timescales using the data collected from 2005 to 2019 which also includes the intensive intra-night monitoring of the target. Additionally, we recorded the brightest flare of the blazar PG 1553 + 113 during April 2019 when the source attained an R-band magnitude of 13.2. Analyzing the spectral evolution of the source during the flare gave a clockwise spectral hysteresis loop and a time lag with V-band variations leading to the R-band ones. Various statistical tests, fitting procedures and cross-correlation techniques are applied to search for periodicity and examine the color-magnitude relationship. We find a median period of (2.21 +/- 0.04) years along with the secondary period of about 210 days. Finally, we briefly discuss various physical mechanisms which are capable of explaining our findings.", 
  "headline": "Optical flux and spectral characterization of the blazar PG 1553+113 based on the past 15 years of data", 
  "identifier": 256847, 
  "image": "https://aperta.ulakbim.gov.tr/static/img/logo/aperta_logo_with_icon.svg", 
  "license": "http://www.opendefinition.org/licenses/cc-by", 
  "name": "Optical flux and spectral characterization of the blazar PG 1553+113 based on the past 15 years of data", 
  "url": "https://aperta.ulakbim.gov.tr/record/256847"
}