UV VARIABILITIES STUDIES IN NGC 4151 SEYFERT 1 AND NGC1068 SEYFERT 2 ACTIVE GALAXIES

UV VARIABILITIES STUDIES IN NGC 4151 SEYFERT 1 AND NGC1068 SEYFERT 2 ACTIVE GALAXIES.

Topics:. AGNs IUE satellite NGC 1068 and its characteristics NGC 4151 and its characteristics UV spectroscopic data and analysis Methodology of UV continuum fluxes, emission lines and absorption lines Objectives Result and discussion.

Topics:. AGNs IUE satellite NGC 1068 and its characteristics NGC 4151 and its characteristics UV spectroscopic data and analysis Methodology of UV continuum fluxes, emission lines and absorption lines Objectives Result and discussion.

AGNs. The galaxies are considered as the “ building blocks” of the universe are said to be “normal galaxies ”. If it is a highly luminous and compact region at the center of the galaxy powered by accretion and super massive black hole are called Active Galactic Nuclei (AGNs). According to Edelson Etal in 1996 the size of the AGN is less than 1017 cm..

Types of Active galaxies:. [image]. [image]. [image].

Seyfert. [image]. [image]. [image]. Quasars. Blazars.

Seyfert. [image]. [image]. [image]. Quasars. Blazars.

Types of Seyfert Galaxies:. [image]. [image]. Quasars.

[image]. [image]. Quasars. Blazars. Radio Galaxies.

The main difference between these graphs are presence of broad emission lines in the spectra. The high speed at which the gas is moving result in broadening of the spectral lines. These broad emission lines gives us important information about the dynamics and properties of the gas near the black hole, helping us to understand the powerful processes happening in Seyfert galaxies. Its like cosmic dance happening right before our eyes..

Quasars. [image].

Quasars. [image]. [image]. [image]. Blazars. Radio Galaxies.

[image]. [image]. [image]. Blazars. Radio Galaxies.

[image]. [image]. [image]. Blazars. Radio Galaxies.

[image]. [image]. [image]. Quasars. Blazars. Radio Galaxies.

[image]. [image]. [image]. Quasars. Blazars. Radio Galaxies.

Characteristics properties of AGNs.

Topics:. AGNs IUE satellite NGC 4151 and its characteristics NGC 1068 and its characteristics UV spectroscopic data and analysis Methodology of UV continuum fluxes, emission lines and absorption lines Objectives Result and discussion.

IUE satellite. International Ultraviolet Explores (IUE), was the first space observatory primarily designed to take (UV) EM spectrum. The IUE was launched successfully on 26 January 1978 from Cape Canaveral, Florida (USA) and very successful observations were made upto September 1996. The IUE satellite was a joint undertaking of NASA (USA), UK Science Research Council (SRC) in collaboration with University College of London (UCL) and the European Space Agency (ESA). It was operated for 16 hours each day, for NASA sponsored observers and for the remaining 8 hours by ESA for ESA and UK sponsored observers..

[image]. [image]. [image].

[image].

Why IUE satellite?. To study the faint objects IUE to obtained the low resolution (~ 8 Å) spectra over a wide UV spectral range (1100 -3200 Å ). To achieve adequate resolution the total spectrum was split into two ranges from 1150 Å to 1950 Å and from 1900 Å to 3200 Å, and so two cameras (SWP and LWP) were required to record the full spectral range..

[image] International Ultraviolet Explorer 370 UlYavi01et Telescope \ NDoIeth•P Upp FenrisDSV.3W.l (Fenris EIIT) Dioscuri-2 Boosters (8) Solar Panels (2) Stacra370 Mass 0.590/02741 lengh 17m 2.2m 17m.

Design. The entrance window of the UVC is magnesium fluoride transparent to wavelengths above 1150 Å and on its inside face is a semi-transparent Cesium-Tellurium photocathode with a quantum efficiency of 10-15% in the UV region, but less than 0.01% in the visible region. The response of a camera to UV photons is nonlinear at high signal levels, owing to saturation effects in the storage of charge in the SEC target. The signal to noise ratio (S/N) of IUE data is dependent on camera and varies greatly with the exposure level and wavelength. The sensitivity of the IUE cameras is determined by the quantum efficiency of the UVC photo cathode, which is highly wavelength dependent..

The sensitivity of the SWP camera increases with wavelength but with a dip near 1500 Å. The IUE data extraction software finally gives absolutely calibrated time integrated fluxes in units of 10-14 erg/cm2/Å. The time-integrated fluxes are converted to usual flux units of erg/cm2/s/Å by dividing it by the total exposure time in seconds. The fundamental standard for the IUE absolute calibration is the flux of eta UMa (HD 120315, mv=1.8)..

NGC 4151 and its characteristics. NGC 4151 HST WFC3 / UVIS F350LP F555W F814W 6.100 light-years 1 , 870 parsecs 20".

The spectrum of NGC 4151 exhibits prominent emission lines, which provide insights into the properties of the ionized gas in the vicinity of the AGN. NGC 4151 exhibits variability in its brightness over time, particularly in the X-ray and ultraviolet parts of the spectrum. This variability is associated with processes occurring in the immediate vicinity of the central black hole. NGC 4151.

Spectral lines. [image] 7.50E-13 5.00E- 13 2.50E-13 -2.50E- 13 1750 2000 2250 D: LWP02132 ore; 30UIZ3 gooo 2500 Wavelength Chs 11 2750 (angstroms) 9250.

Topics:. AGNs IUE satellite NGC 4151 and its characteristics NGC 1068 and its characteristics UV spectroscopic data and analysis Methodology of UV continuum fluxes, emission lines and absorption lines Objectives Result and discussion.

NGC 1068 and its characteristics:. Constellation Cetus Right Ascension (RA) 02h 42m 40.771s Declination (Dec) -00ο 00ʹ 47.84ʹʹ Distance (d) 47 million Ly (14 Mpc) Redshift (z) 1137±3 km/s Apparent magnitude (m) 8.9 Type Spiral and Seyfert 2 active galaxy Mass ̴109 Msun.

Observational Significance NGC 1068 is one of the nearest and best-studied examples of Seyfert galaxies. One of the closest and brightest Spectacular object. NGC 1068 helps to the scientist to understand the mechanism behind the Energetic Emission and interaction between the black hole and Surrounding gas and dust..

NGC 1068 is a well-studied galaxy due to its proximity and the prominence of its AGN. It serves as a valuable laboratory for understanding the connections between supermassive black holes, galactic dynamics, and the broader cosmic environment. NGC 1068 has been studied across various wavelengths, including optical, infrared, radio, and X-ray. Observations at different wavelengths help astronomers understand different aspects of the galaxy, from the distribution of stars to the nature of the AGN..

Topics:. IUE satellite NGC 4151 and its characteristics UV spectroscopic data and analysis Methodology of UV continuum fluxes, emission lines and absorption lines Objectives Result.

[image]. Spectroscopic study of AGNs.

Methodology of uv continuum flux emission line.

Line and Continuum Flux Measurements.

We use two methods to analysis, one is using IRAF and another is using python . IRAF is a collection of a software written at National Optical Astronomy Observatory (NOAO) geared towards the reduction of astronomical images the reduction of astronomical image in pixel array form..

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Spectroscopic data. We took spectroscopic data from IUE satellites and converted in the form of fits file for example “dcdr2dlwp00505mxlo.fits” here dc= doppler corrected dr= reddening corrected 2d= 2 dimensional converted spectrum spectrum id =This is typically depending on the camera i.e. SWP,LWP and LWR mxlo= standard format as recorded by IUE fits= standard fits format..

Using IRAF. The continuum measurement task of IRAF gives the mean continuum flux value over the 50 Å wide window and the rms deviation of the measurement flux from the mean flux, which is considered as the most probable uncertainty in the continuum flux measurements. The Signal to Noise Ratio (SNR) of the IUE camera ranges between  3 - 40. We have selected the continuum measurements for which the SNR  5 and hence the maximum amount of uncertainty in the continuum measurements is 20%..

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But it takes times. we can look for many windows as much we can..

Spectral data analysis using python code: We change the spectrum format means fits into txt format. We choose the good windows using IRAF and their corresponding line from txt and fixed it in the code. Using code we can analyse the spectral data.

dcdr2dlwp00505mxlo. txt 'dcdr2dlwp00505mxlo.txt_conttnuum subtratton_Mg.png' 'dcdr2dlwp00505mxlo. txt_MgII fitting.png' ' Mgll power-law. ' $ python3 'IWP Mgll power-law. NCC4151.VHD.RC.py' Please enter the file you want to opendcdr2dlwp00505mxlo. txt Please enter the name of the source as you want it to appear on the plotsdcdr2dlwp00505nx10i txt [[Model]] [[Ftt Statistics]] # fitting method : leastsq # function evals # data points # variables chi-square : 2.8421+27 reduced chi-square - - 3.8407+29 Akaike info crit : -4970.65449 Bayesian info crit •4965.99303 R•squared : I.ooeeeooo [[Vartables]] amplitude: 4.6091+10+1. (192.03%) (init : le.09) index: -1.14312293 +1.0.24189288 (21.16%) (init 7) [[Correlattons]] (unreported correlations are < 0.100) C(amplttude, index) - - .l.eoeo Activities 8 Terminal Is : 95 : 76 oct23 9:32PM n [email protected]: *Pesktop/test3 Mgll_powerlaw fit. csv'.

- -SNR: Window 2601 : 2651 2699:2750 2931 :2951 2999 : 3049 [ [Model]] Favg 5.68318e-14 5.44977e-14 5.02275e-14 4.83686e-14 F rms SNR 7 .19134e-15 7.75703e-15 2.87213e-15 5.42672e-15 7.9628 7 . 02559 17 .4879 8.91305 Model (sumGauss) [[Ftt Statistics]] # fitting method = leastsq # function evals 198 # data points = 169 # variables cht- square = 6.3502e-27 reduced chi-square - - 3.8958e-29 Akaike info crit -11049.2547 Bayesian info crit - - -11636.4753 R-squared 1. ooeeeoee [ [Variables]] Sl: 4.21172262 +/- kl: 5.4809e-14 +/- mi: 2798.02352 +1- 0.40829145 (0.01%) (init mz: 2792.35377 +/- 1.66438766 (0.06%) (init 0.46674305 (11.08%) (init = 3) s2: 32.2130920 +/- 1.83922270 (5.71%) (init = 8) 4.8843+15 (8.91%) (init k2: 3.7901e-14 +1- 2.3640e-15 (6.24%) (intt = 2800) = 2800) = 1.2e-14) = 1.2e-14) [ [Correlations]] (unreported correlations are < lee) C(S2, C(SI, C(kl, C(SI, C(SI, C(S2, C(m2, C(mz, C(ml, C(m2, k2) k2) - -o. k2) = -O. kl) = -e. kl) - +0. k2) = +0.1409 kl) = -e. -Equivalent The EW Of Mg1 The EW of mg2 6946 = -0.4931 3555 3146 2881 2487 1379 = -0.1186 1017 width: = 10.938628 (+-1.55553) Angstrom = 57.719633 (+-4.88078) Angstrom The EW of full mg = 68.658261 (+-6.43632) Angstrom -- -Fluxes of components: The Flux Of Mg1 = 5.78593+13(+-3.2827e-14) erg/s/cmA2 The Flux of mg2 = 3.06034e-12(+-1.0324e-13) erg/s/cmA2 The Flux Of full Mg = 3.63893e-12 (+-1.36e67e-13) erg/s/cmA2 -FWHMS The FWHM of Mg(l) = 9.931625 Angstrom The FWHM of mg(l) = 1063.376601 Km/s The FWHM of mg(2) = 75.856489 Angstrom The FWHM of mg(2) = 8121.935141 Km/s The FWHM of mg(BOTH) = 15.704255 Angstrom The FWHM of mg(BOTH) = 1681.450615 Km/s chengIet@chengIet-IdeaPad : - / Desk top/ tes tJS.

[image] /home/chenglei/Desktop/2023-NGC4151-lwp-txt-data/dcdr2dlwp00505mxlo.txt Q) le—13 1.4 1.2 1.0 0.8 0.6 0.4 0.2 0.0 2600 Before continuum subtraction continuum level Continuum windows After continuum subtraction 2700 2800 2900 3000 Wavelength (A).