Image Reduction And Analysis Facility Research Articles

Inspecting PGC 165324 and PGC 977941 Galaxies Using a Combination ofPhotometric and Spectroscopic Methods

Photometric and spectroscopic approaches were utilized to examine the two galaxies, PGC 165324 and PGC 977941. Data releases (DR7 and DR17) from "The Sloan Digital Sky Survey (SDSS)” were employed to acquire the observed data. Then, ellipsoids were fitted via employing the Image Reduction and Analysis Facility (IRAF) with utilising STSDAS Library, the ELLIPS task. Along with the astrometric characteristics, the surfaces’ brightness of the galaxies PGC 165324 and PGC 977941, as well as their magnitudes, cumulative flux, central axis position angles, ellipticities, vertical and horizontal shifts, isophotal shape variables (B4), and also the star-forming rates (SFRs), were analysed and evaluated. It was indicated that the two galaxies, are members of a close pair galaxy system; in addition, they are considered a physical system; the PGC 165324 galaxy was a merging galaxy with a higher SFR. It was likely that the PGC 977941 had separated itself from the galaxy collision and drifted away.

شرح الخواص الضوئية والطيفية للزوج المجري Sip-39

تمت دراسة الزوج المجري Sip-39 باستخدام طرق القياس الضوئي والطيفي. البيانات الرصدية اخذت من اصدار البيانات السابع عشر (DR17) من "Sloan Digital Sky Survey (SDSS)" وتمت عمل ال fitting لصور المجرتين باستخدام برنامج (IRAF) من خلال المكتبةSTSDAS باستخدام ELLIPS task.تم دراسة وحساب كل من اللمعان السطحي للمجرتين في الزوج ، بالإضافة إلى الانبعاث الكلي ، وشكل القطع الناقص ، وزوايا انحراف المحور الكبير، الانحرافات العمودية والأفقية ، ومعاملات كيرشوف للشكل (B4)، والاقدار ، ومعدلات تشكل النجوم (SFR) ، بالإضافة إلى خواص القياسات الفلكية للزوج ، حيث ظهر من خلال تحليل البيانات أن زوج Sip-39 هو قريب مع علامات تفاعل واضحة ، ويعتبر نظامًا فيزيائيا مع معدلات محسنة ل .SFR

Study of aerosol content based on spectrophotometric observations: A comparison with long-term extinction profile from photometric observations

Spectroscopic observations of standard stars (spectrophotometric) have been carried out at Bosscha Observatory ITB (latitude= 6°49′28″ S, longitude= 107°36′56″ E, altitude=1310 m) using the Celestron C-11 reflector (D=11 inches, F/10.0), equipped with NEO R-1000 spectrograph (Resolution of 1000), and ST-8XME CCD camera to deduce total atmospheric extinction curve. Spectrograms were reduced with the long-slit task in the Image Reduction and Analysis Facility (IRAF). The total extinction curve obtained from observation is decomposed into three main components, i.e. Rayleigh scattering, Ozone and water vapor absorptions, and extinction by aerosol. The extinction profile by Aerosol serves as an important indication on size and distribution of particulates as the main constituent of atmospheric pollutant. This pollutant can be resulted from natural process or anthropogenic activities. The behavior of atmospheric extinction over Bosscha Observatory based on long-term astronomical photometric database (1982-1993) was previously studied by one of us in 1993. In this study we analyze new data and study the dynamics of atmosphere by comparing our recent result with that from long-term photometric observations to indicate variation of degree of atmospheric turbidity, particulate size and its distribution over the atmosphere. We recommend that long-term regular based spectrophotometry at an Observatory is imperative as an effective means to gain our insight on atmospheric dynamic.

Spectroscopic observations of emission-line objects at Bosscha Observatory

We report an optical spectroscopic observational program of emission-line objects at Bosscha Observatory. The observations were conducted on 18 nights between May to July 2019. We employ the spectrograph NEO-R1000 (R∼1000) equipped with SBIG ST-8 XME CCD camera attached to a 28 cm (F/10) telescope and the spectrograph LHIRES III (R∼5000) equipped with SBIG ST-402 CCD camera attached to a 25 cm (F/10) telescope. Data reduction has been carried out using longslit transform routines within the Image Reduction and Analysis Facility (IRAF). We have successfully obtained the spectra of 9 Wolf-Rayet (WR) stars, 13 B-emission (Be) stars, 2 Luminous Blue Variable (LBV) stars, 8 Herbig Ae/Be (HAeBe) stars, and 1 recurrent nova. The obtained spectra are presented and discussed in this paper.

Surface Photometry of NGC 3 Lenticular Galaxy

Lenticular galaxy NGC3 has been chosen to study the surface photometry using griz filter. The data where obtained from the seventh Sloan Digital Sky Survey (SDSS) Data Release seven (DR7), and main the image reduction was done by the pipeline of SDSS. The work was achieved by the ELLIPS task from the STSDAS ISOPHOTE package in the Image Reduction and Analysis Facility (IRAF).The overall structure of the galaxy (a bulge, a bar, isophotal contour maps, together with a bulge to disk decomposition of the galaxy images where achieved, Also, the photometric properties (the disk position angle, ellipticity, B4 and inclination of the galaxy) where estimated.

Theoretical investigation for the relation (supermassive black hole mass)–(spiral arm pitch angle): a correlation for galaxies with classical bulges

In this work, the determination of the masses of supermassive black holes (SMBHs) and the properties of their host spiral galaxies are focused for the purposes of constraining scaling relations and with the aim of understanding the role of SMBHs in the evolution of galaxies.The measurements of SMBHs mass for a sample of 40 spiral galaxies were studied by applying indirect techniques (the SMBHs mass versus stellar/gas velocity dispersion relation). In addition, spiral arm pitch angle of a sample of nearly face-on spiral galaxies were measured using IRAF (The Image Reduction and Analysis Facility) and two-dimensional Fast Fourier Transform (2DFFT) program.Finally, we present a new correlation between spiral arm pitch angle (a measure of the tightness of spiral structure) and the mass of supermassive black holes (BHs) in the nuclei of classical galaxies.

Effect of Active Galactic Nuclei (AGN) on the Photometric and Morphologic Properties of NGC 4414 and NGC 4369 Spiral Galaxies

The purpose of this work is to clarify the effect of the Active Galactic Nucleus (AGN) on the properties of the galaxy. A photometric study of two galaxies by surface optical measurements techniques and by using'griz filters' was performed. The scientific material that used in this work was obtained from ''SLOAN DIGITAL SKY SURVEY'' (DR7), a fuzzy color, contour maps, photometric parameters, and color indices were studied by using surface photometric technique. The work was done by Ellipse task in IRAF (Image Reduction and Analysis Facility) software from the National Optical Astronomy Observatory (NOAO).

Solvepol: A Reduction Pipeline for Imaging Polarimetry Data

We present a newly, fully automated, data pipeline, Solvepol, designed to reduce and analyze polarimetric data. It has been optimized for imaging data from the Instituto de Astronomía, Geofísica e Ciências Atmosféricas (IAG) of the University of São Paulo (USP), calcite Savart prism plate-based IAGPOL polarimeter. Solvepol is also the basis of a reduction pipeline for the wide-field optical polarimeter that will execute SOUTH POL, a survey of the polarized southern sky. Solvepol was written using the Interactive data language (IDL) and is based on the Image Reduction and Analysis Facility (IRAF) task PCCDPACK, developed by our polarimetry group. We present and discuss reduced data from standard stars and other fields and compare these results with those obtained in the IRAF environment. Our analysis shows that Solvepol, in addition to being a fully automated pipeline, produces results consistent with those reduced by PCCDPACK and reported in the literature.

Infrared-faint radio sources are at high redshifts

Context: Infrared-Faint Radio Sources (IFRS) are characterised by relatively high radio flux densities and associated faint or even absent infrared and optical counterparts. The resulting extremely high radio-to-infrared flux density ratios up to several thousands were previously known only for High-redshift Radio Galaxies (HzRGs), suggesting a link between the two classes of object. Prior to this work, no redshift was known for any IFRS in the Australia Telescope Large Area Survey (ATLAS) fields which would help to put IFRS in the context of other classes of object, especially of HzRGs. Aims: This work aims at measuring the first redshifts of IFRS in the ATLAS fields. Further, we test the hypothesis that IFRS are similar to HzRGs, as higher-redshift or dust-obscured versions of these massive galaxies. Methods: A sample of IFRS was spectroscopically observed using the Focal Reducer and Low Dispersion Spectrograph 2 (FORS2) at the Very Large Telescope (VLT). The data were calibrated based on the Image Reduction and Analysis Facility (IRAF) and redshifts extracted. This information was then used to calculate rest-frame luminosities, and to perform the first spectral energy distribution modelling of IFRS based on redshifts. Results: We found redshifts of 1.84, 2.13, and 2.76, for three IFRS, confirming the suggested high-redshift character of this class of object. These redshifts as well as the resulting luminosities show IFRS to be similar to HzRGs. We found further evidence that fainter IFRS are at even higher redshifts. Conclusions: Considering the similarities between IFRS and HzRGs substantiated in this work, the detection of IFRS, which have a significantly higher sky density than HzRGs, increases the number of Active Galactic Nuclei in the early universe and adds to the problems of explaining the formation of supermassive black holes shortly after the Big Bang.

Observing and Reducing IFUs: INTEGRAL and PMAS—Properties of the Ionized Gas in HH 202

The reduction of integral field spectroscopy (IFS) data requires several stages and many repetitive operations to convert raw data into, typically, a large number of spectra. Instead there are several semiautomatic data reduction tools and here we present this data reduction process using some of the Image Reduction and Analysis Facility (IRAF) tasks devoted to reduce spectroscopic data. After explaining the whole process, we illustrate the power of this instrumental technique with some results obtained for the object HH202 in the Orion Nebula (Mesa-Delgado et al., 2009).

The Processing and Classification for the Spectra of Six Comets

In order to explore the relationship between comets and asteroids, the spectra of six comets, including 78P, C/2009 P1, 49P, C/2010 G2, C/2010 S1, and C/2011 F1, have been observed with the 2.16 m telescope at the Xinglong Observing Station of National Astronomical Observatories. At the same time, the spectra of some sun-like stars are also observed. The IRAF (Image Reduction and Analysis Facility) software is used to process the obtained spectra, and to obtain the relative reflectance spectra of the six comets. Then, they are compared with the 24 asteroid spectral types of the Bus-DeMeo taxonomy to derive the spectral distances of these comets. According to the order of the calculated spectral distances, the details of the reflectance spectra, as well as the results of the K-S test, the asteroid spectral types which are most close to the spectra of these comets are finally determined.

A MULTI-DIMENSIONAL REDUCTION METHOD OF LARGE-SCALE SURVEY DATABASE

We present a multi-dimensional reduction method of the surveyed cube database obtained using a single- dish radio telescope in Taeduk Radio Astronomy Observatory (TRAO). The multibeam receiver system installed at the 14 m telescope in TRAO was not optimized at the initial stage, though it became more stabilized in the following season. We conducted a Galactic Plane survey using the multibeam receiver system. We show that the noise level of the first part of the survey was higher than expected, and a special reduction process seemed to be definitely required. Along with a brief review of classical methods, a multi-dimensional method of reduction is introduced; It is found that the 'background' task within IRAF (Image Reduction and Analysis Facility) can be applied to all three directions of the cube database. Various statistics of reduction results is tested using several IRAF tasks. The rms value of raw survey data is 0.241 K, and after primitive baseline subtraction and elimination of bad channel sections, the rms value turned out to be 0.210 K. After the one-dimensional reduction using 'background' task, the rms value is estimated to be 0.176 K. The average rms of the final reduced image is 0.137 K. Thus, the image quality is found to be improved about 43% using the new reduction method.

An automatic data‐reduction pipeline for fixed‐format Echelle spectrographs: First results

Our data-reduction pipeline is based on the NOAO Image Reduction and Analysis Facility (IRAF). It consists of a number of IRAF-CL scripts which are invoked by a master script (see Ritter & Washuettl 2002 for more details). The subtasks access a parameter file where all relevant IRAF parameters are stored. If a particular parameter is not found in the parameter file (or the parameter file itself is not present or accessible), standard parameters, which are stored in the subtasks, are used. Four reference files are needed for cleaning the images of bad pixels, for defining the position of the Echelle orders on the CCD, for identifying Th-Ar emission lines for the wavelength calibration and for the radial-velocity measurement (which is not implemented yet in the pipeline because of missing reference star spectra for the individual types of stars).

A FAST REDUCTION METHOD OF SURVEY DATA IN RADIO ASTRONOMY

We present a fast reduction method of survey data obtained using a single-dish radio telescope. Along with a brief review of classical method, a new method of identification and elimination of negative and positive bad channels are introduced using cloud identification code and several IRAF (Image Reduction and Analysis Facility) tasks relating statistics. Removing of several ripple patterns using Fourier Transform is also discussed. It is found that BACKGROUND task within IRAF is very efficient for fitting and subtraction of base-line with varying functions. Cloud identification method along with the possibility of its application for analysis of cloud structure is described, and future data reduction method is discussed.

The Global Oscillation Network Group (GONG)

As a community facility, the National Solar Observatory is establishing a six-site ground-based solar observing network around the world. This Global Oscillation Network Group (GONG) aims at essentially continuous imaged observations of global solar oscillations for a minimum of three years. Resulting data will be used to study the solar interior using helioseismology. The heart of the observing instrument is a thermally compensated, wide-field Fourier Techometer operated automatically by a computer control system. Data from the six GONG stations is expected to total over one gigabyte per day. Pipeline processing of these data will proceed contemporaneously, reducing the raw data to several standard product data sets at sustained throughput rates in excess of 6 megaflops and peak rates that may exceed 50 megaflops. In support of widespread scientific participation, software analysis tools based on the Image Reduction and Analysis Facility ( IRAF) and data distribution will be provided. Science teams have been formed and are actively supporting the project. The field instrument will reach the prototype stage in early 1989 and full operation of the network is expected in 1992.