title: ÐÑÑÐ»ÐµÐ´Ð¾Ð²Ð°Ð½Ð¸Ðµ ÑÐ¿ÐµÐºÑÑÐ¾Ð² Ð¼Ð¾Ð»ÐµÐºÑÐ»ÑÑÐ½ÑÑ Ð¾Ð±Ð»Ð°ÐºÐ¾Ð² Ð² ÐÐ¾Ð»ÑÑÐ¾Ð¼ Ð¸ ÐÐ°Ð»Ð¾Ð¼ ÐÐ°Ð³ÐµÐ»Ð»Ð°Ð½Ð¾Ð²ÑÑ ÐÐ±Ð»Ð°ÐºÐ°Ñ Ð½Ð° Ð¿ÑÐµÐ´Ð¼ÐµÑ Ð½Ð°Ð»Ð¸ÑÐ¸Ñ Ð»Ð¸Ð½Ð¸Ð¹ Ð´ÐµÐ¹ÑÐµÑÐ¸ÑÐ¾Ð²Ð°Ð½Ð½Ð¾Ð³Ð¾ Ð²Ð¾Ð´Ð¾ÑÐ¾Ð´Ð° HD Ð¸ Ð¿Ð¾ÑÐ»ÐµÐ´ÑÑÑÐ¸Ð¹ Ð°Ð½Ð°Ð»Ð¸Ð· Ð¿Ð¾Ð»ÑÑÐµÐ½Ð½ÑÑ Ð´Ð°Ð½Ð½ÑÑ , Ð° ÑÐ°ÐºÐ¶Ðµ Ð¿Ð¾Ð»ÑÑÐµÐ½Ð¸Ðµ Ð¾ÑÐµÐ½ÐºÐ¸ Ð¾ÑÐ½Ð¾ÑÐ¸ÑÐµÐ»ÑÐ½Ð¾Ð¹ ÑÐ°ÑÐ¿ÑÐ¾ÑÑÑÐ°Ð½ÐµÐ½Ð½Ð¾ÑÑÐ¸ Ð´ÐµÐ¹ÑÐµÑÐ¸ÑÐ¾Ð²Ð°Ð½Ð½Ð¾Ð³Ð¾ Ð²Ð¾Ð´Ð¾ÑÐ¾Ð´Ð° hd/h
title: Ð²ÑÐ¿ÑÑÐºÐ½Ð°Ñ ÐºÐ²Ð°Ð»Ð¸ÑÐ¸ÐºÐ°ÑÐ¸Ð¾Ð½Ð½Ð°Ñ ÑÐ°Ð±Ð¾ÑÐ° Ð±Ð°ÐºÐ°Ð»Ð°Ð²ÑÐ°
titleType: Subtitle
title: Investigation of the spectra of the interstellar medium of the Large and Small Magellanic Clouds in order to search for HD molecules
Creators: name: ÐÐ»Ð¾ÑÐ½Ð¸ÐºÐ¾Ð², ÐÐµÐ¾ÑÐ³Ð¸Ð¹
Publisher: name: Ð¡Ð°Ð½ÐºÑ-ÐÐµÑÐµÑÐ±ÑÑÐ³ÑÐºÐ¸Ð¹ Ð¿Ð¾Ð»Ð¸ÑÐµÑÐ½Ð¸ÑÐµÑÐºÐ¸Ð¹ ÑÐ½Ð¸Ð²ÐµÑÑÐ¸ÑÐµÑ ÐÐµÑÑÐ° ÐÐµÐ»Ð¸ÐºÐ¾Ð³Ð¾
Year: 2022
Subjects: ÐºÐ¾ÑÐ¼Ð¾Ð»Ð¾Ð³Ð¸Ñ
Ð¼Ð¾Ð»ÐµÐºÑÐ»ÑÑÐ½Ð¾Ðµ Ð¾Ð±Ð»Ð°ÐºÐ¾
ÑÐ¿ÐµÐºÑÑÐ¾-ÑÐºÐ¾Ð¿Ð¸Ñ
Ð¼Ð¾Ð´ÐµÐ»Ð¸ÑÐ¾Ð²Ð°Ð½Ð¸Ðµ
Ð´ÐµÐ¹ÑÐµÑÐ¸
cosmology
molecular cloud
spectroscopy
modeling
deuterium

description: Ð¢ÐµÐ¼Ð° Ð²ÑÐ¿ÑÑÐºÐ½Ð¾Ð¹ ÐºÐ²Ð°Ð»Ð¸ÑÐ¸ÐºÐ°ÑÐ¸Ð¾Ð½Ð½Ð¾Ð¹ ÑÐ°Ð±Ð¾ÑÑ: Â«ÐÑÑÐ»ÐµÐ´Ð¾Ð²Ð°Ð½Ð¸Ðµ ÑÐ¿ÐµÐºÑÑÐ¾Ð² Ð¼Ð¾Ð»ÐµÐºÑÐ»ÑÑÐ½ÑÑ Ð¾Ð±Ð»Ð°ÐºÐ¾Ð² Ð² ÐÐ¾Ð»ÑÑÐ¾Ð¼ Ð¸ ÐÐ°Ð»Ð¾Ð¼ ÐÐ°Ð³ÐµÐ»Ð»Ð°Ð½Ð¾Ð²ÑÑ ÐÐ±Ð»Ð°ÐºÐ°Ñ Ð½Ð° Ð¿ÑÐµÐ´Ð¼ÐµÑ Ð½Ð°Ð»Ð¸ÑÐ¸Ñ Ð»Ð¸Ð½Ð¸Ð¹ Ð´ÐµÐ¹ÑÐµÑÐ¸ÑÐ¾Ð²Ð°Ð½Ð½Ð¾Ð³Ð¾ Ð²Ð¾Ð´Ð¾ÑÐ¾Ð´Ð° HD Ð¸ Ð¿Ð¾ÑÐ»ÐµÐ´ÑÑÑÐ¸Ð¹ Ð°Ð½Ð°Ð»Ð¸Ð· Ð¿Ð¾Ð»ÑÑÐµÐ½Ð½ÑÑ Ð´Ð°Ð½Ð½ÑÑ, Ð° ÑÐ°ÐºÐ¶Ðµ Ð¿Ð¾Ð»ÑÑÐµÐ½Ð¸ÐµÐ¾ÑÐµÐ½ÐºÐ¾Ð¹ Ð¾ÑÐ½Ð¾ÑÐ¸ÑÐµÐ»ÑÐ½Ð¾Ð¹ ÑÐ°ÑÐ¿ÑÐ¾ÑÑÑÐ°Ð½ÐµÐ½Ð½Ð¾ÑÑÐ¸ Ð´ÐµÐ¹ÑÐµÑÐ¸ÑÐ¾Ð²Ð°Ð½Ð½Ð¾Ð³Ð¾ Ð²Ð¾Ð´Ð¾ÑÐ¾Ð´Ð° HD/HÂ».Â Ð¦ÐµÐ»ÑÑ Ð´Ð°Ð½Ð½Ð¾Ð¹ ÑÐ°Ð±Ð¾ÑÑ ÑÐ²Ð»ÑÐµÑÑÑ Ð¸ÑÑÐ»ÐµÐ´Ð¾Ð²Ð°Ð½Ð¸Ðµ ÑÐ¿ÐµÐºÑÑÐ¾Ð² Ð¸Ð·Ð»ÑÑÐµÐ½Ð¸Ð¹ ÑÑÐ´Ð° Ð¾Ð±ÑÐµÐºÑÐ¾Ð², Ð½Ð°ÑÐ¾Ð´ÑÑÐ¸ÑÑÑ Ð² ÐÐ°Ð³ÐµÐ»Ð»Ð°Ð½Ð¾Ð²ÑÑ ÐÐ±Ð»Ð°ÐºÐ°Ñ. Ð¡ Ð¿Ð¾Ð¼Ð¾ÑÑÑ ÑÐ¿ÐµÑÐ¸Ð°Ð»ÑÐ½Ð¾Ð¹ Ð¿ÑÐ¾Ð³ÑÐ°Ð¼Ð¼Ñ (spectro, ÑÐ·ÑÐº python) ÑÐ¿ÐµÐºÑÑÑ, Ð²Ð·ÑÑÑÐµ Ñ ÑÐ°Ð¹ÑÐ° Ð¼Ð¸ÑÑÐ¸Ð¸ FUSE (far ultraviolet spectroscopic explorer), Ð±ÑÐ»Ð¸ Ð¾Ð±ÑÐ°Ð±Ð¾ÑÐ°Ð½Ñ Ð¼ÐµÑÐ¾Ð´Ð¾Ð¼ Ð¿Ð¾ÑÑÑÐ¾ÐµÐ½Ð¸Ñ B-ÑÐ¿Ð°Ð»Ð¹Ð½Ð° Ð¸ Ð´Ð°Ð»ÑÐ½ÐµÐ¹ÑÐµÐ³Ð¾ ÑÐ¸ÑÐ¸ÑÐ¾Ð²Ð°Ð½Ð¸Ñ. ÐÐ· Ð¿Ð¾Ð»ÑÑÐµÐ½Ð½ÑÑ Ð´Ð°Ð½Ð½ÑÑ ÑÐ»ÐµÐ´ÑÐµÑ, ÑÑÐ¾ Ð² ÐÐ°Ð³ÐµÐ»Ð»Ð°Ð½Ð¾Ð²ÑÑ Ð¾Ð±Ð»Ð°ÐºÐ°Ñ Ð´ÐµÐ¹ÑÑÐ²Ð¸ÑÐµÐ»ÑÐ½Ð¾ Ð¿ÑÐ¸ÑÑÑÑÑÐ²ÑÑÑ Ð¼Ð¾Ð»ÐµÐºÑÐ»Ñ Ð´ÐµÐ¹ÑÐµÑÐ¸Ñ HD. ÐÐ»Ñ ÑÑÐ´Ð° Ð¾Ð±ÑÐµÐºÑÐ¾Ð² Ð±ÑÐ»Ð¸ Ð¿Ð¾Ð»ÑÑÐµÐ½Ñ Ð»ÑÑÐµÐ²ÑÐµ ÐºÐ¾Ð½ÑÐµÐ½ÑÑÐ°ÑÐ¸Ð¸ (Ð»Ð¸Ð±Ð¾ Ð¸Ñ Ð²ÐµÑÑÐ½Ð¸Ðµ Ð³ÑÐ°Ð½Ð¸ÑÑ).Â ÐÐ»Ñ ÑÐ¿ÐµÐºÑÑÐ¾Ð² Ð¾ÑÑÐ°Ð»ÑÐ½ÑÑ Ð¾Ð±ÑÐµÐºÑÐ¾Ð² ÑÐ»Ð¾Ð¶Ð½Ð¾ ÑÑÑÐ°Ð½Ð¾Ð²Ð¸ÑÑ Ð½Ð°Ð»Ð¸ÑÐ¸Ðµ Ð»Ð¸Ð½Ð¸Ð¹ Ð¿Ð¾Ð³Ð»Ð¾ÑÐµÐ½Ð¸Ñ Ð¼Ð¾Ð»ÐµÐºÑÐ» HD Ð¸Ð·-Ð·Ð° ÑÑÐ´Ð° ÑÐ°ÐºÑÐ¾ÑÐ¾Ð²: Ð½Ð¸Ð·ÐºÐ°Ñ ÐºÐ¾Ð½ÑÐµÐ½ÑÑÐ°ÑÐ¸Ñ Ð¼Ð¾Ð»ÐµÐºÑÐ» H2 (ÐºÐ¾Ð½ÑÐµÐ½ÑÑÐ°ÑÐ¸Ñ HD Ð¿ÑÐ¸Ð¼ÐµÑÐ½Ð¾ Ð½Ð° 5 Ð¿Ð¾ÑÑÐ´ÐºÐ¾Ð² Ð¼ÐµÐ½ÑÑÐµ, ÑÐµÐ¼ H2), Ð²ÑÑÐ¾ÐºÐ¾Ðµ Ð¾ÑÐ½Ð¾ÑÐµÐ½Ð¸Ðµ Ð¿Ð¾Ð¼ÐµÑ Ð½Ð° ÑÐ¿ÐµÐºÑÑÐµ Ðº ÑÐ°Ð·Ð¼ÐµÑÐ°Ð¼ Ð°Ð±ÑÐ¾ÑÐ±ÑÐ¸Ð¾Ð½Ð½ÑÑ Ð»Ð¸Ð½Ð¸Ð¹.
description: The topic of the final qualifying work: Â«Investigation of molecular cloud spectra in Large and Small Magellanic Clouds for the presence of HD deuterated hydrogen lines and subsequent analysis of the data obtained, as well as obtaining an estimate of the relative prevalence of HD/H deuterated hydrogenÂ».Â The purpose of this work is to study the emission spectra of a number of objects located in the Magellanic Clouds. With the help of a special program (spectro, python language), the spectra taken from the FUSE mission site (far ultraviolet spectroscopic explorer) were processed by the method of constructing a B-spot and further fitting. From the data obtained, it was noticed that deuterium HD absorption lines are indeed present in the Magellanic clouds. Radiation concentrations (or their upper limits) were also obtained for a number of objects.Â For other objects, it is difficult to establish the presence of absorption lines of HD molecules due to a number of factors: low concentration of H2 molecules (HD concentration is about 5 orders of magnitude less than H2), inaccurate telescope resolution values, strong noise on some spectra.