BIBECHANA 18 (2) (2021) 154-163 154 BIBECHANA ISSN 2091-0762 (Print), 2382-5340 (Online) Journal homepage: http://nepjol.info/index.php/BIBECHANA Publisher: Department of Physics, Mahendra Morang A.M. Campus, TU, Biratnagar, Nepal Distribution of dust properties around carbon rich AGB star: IRAS 04427+4951 using IRIS and AKARI survey Devendra Raj Upadhyay1*, Trishna Subedi 1 1Department of Physics, Amrit Campus, Tribhuvan University, Kathmandu, Nepal *Email: devendra.upadhyaya@ac.tu.edu.np Article Information: Received: March 3, 2021 Accepted: June 8, 2021 Keywords: Dust color temperature Inclination angle Extinction ABSTRACT Interstellar dust plays a vital role in the interstellar medium, and their properties using far-infrared bands analyze nature around asymptotic giant branch stars and other stellar objects. Here, we present physical properties across the cavity region around an AGB star named IRAS 04427+4951 using Sky View Observatory of IRIS, AKARI map, SIMBAD, Aladin v2.5, and Gaia Archive. The average dust color temperature and mass are 23.48 ± 0.009 K, 3.55×1027 kg (1.79× 10-3 Mʘ ) using IRIS data and 14.89±0.004 K and 5.34×1028 kg (2.69 × 10−2Mʘ ) from AKARI data. The size of isolated cavity-like structure around the AGB stars of 45.67 pc × 17.02 pc and 42.25 pc × 17.76 pc, respectively. The visual extinction is to be in the range of 3.2×10-4 to 4.3×10- 4 mag obtained using IRIS survey and 4.5 × 10-3 to 7.4×10-3 mag from AKARI survey. The inclination angle is 86.150 and 86.080. The results we present gives the dust distributions, their properties and role which is useful for the study of visual extension phenomena and astrochemistry of interstellar medium. DOI: https://doi.org/10.3126/bibechana.v18i2.35394 This work is licensed under the Creative Commons CC BY-NC License. https://creativecommons.org/licenses/by-nc/4.0/ 1. Introduction The interstellar medium plays a vital role that enables structures in the space between the stars in galaxies [1, 2]. The physics and astrochemistry around low and intermediate massive stars (0.8 - 8) Mʘ [3] in Milky-way and other galaxies will enhance research up to polyaromatic hydrocarbon, carbon nanotube in space, and more [2]. These stars evolve and become Asymptotic Giant Branch (AGB) stars having approximately luminous intensity (Lstar=104 Lʘ), surface temperature (Teff =3000 K), radius (Rstar =1 AU), having mass rates (10-7 to a few number times 10-4Mʘ/yr) [4, 5]. A dusty environment like flux distribution, dust color temperature, Planck function, dust mass, size of the structure and inclination angle of cavity-like structure the Far Infrared loop, KK loop and pulsar candidate investigated by Jha et al. [6, 7] using both improved reprocessing of IRAS(IRIS) and AKARI survey they obtained the nearly inverse relationship between dust mass and temperature. The environment around Planetary nebulae: NGC 1514, NGC 6826, NGC 2899, and Cone like mailto:devendra.upadhyaya@ac.tu.edu.np https://doi.org/10.3126/bibechana.v18i2.35394 https://creativecommons.org/licenses/by-nc/4.0/ http://nepjol.info/index.php/BIBECHANA Devendra Raj Upadhyay and Trishna Subedi/BIBECHANA 18 (2) (2021) 154-163 155 asymmetrical dust structure studied by using IRAS 12, 25, 60, and 100 can not be visible by the necked eye, but their heating effect can felt. Here, we have present our work related to cavities regions around AGB stars by comparing two survey: IRIS and AKARI . So it is new work to understand Far Infrared features around AGB stars. This work based on revised catalog of C-rich AGB stars categorized by Suh & Hong(2017) [16] and it includes a comparative study of dust features. This work present in four sections first introduction, second methods, third results and discussion, and the fourth one is the conclusion. 2. Methodology We have taken data of AGB stars using A catalog of AGB stars in our Galaxy (http://web.chungbuk.ac.kr/~kwsuh/agb.html) presented by Shu et al. [16-19]. His group presented a revised catalog of 3828 O-rich AGB stars and 1168 C-rich AGB stars. We have verified data using SIMBAD Astronomical Database - CDS (Strasbourg) (http://simbad.u-strasbg.fr/simbad/), Sky View Virtual Observatory (https://skyview.gsfc.nasa.gov/current/cgi/query.pl), Infrared Astronomical Satellite, IRIS - Improved Reprocessing of the IRAS Survey, AKARI survey. The distance of the candidate is taken from Gaia Archive (https://gea.esac.esa.int/archive/). We carried out search of different cavity like structures around the different AGB stars in IRIS and AKARI map available in the sky view virtual observatory. The steps that we followed during the search are elaborated below: Step-I: Inspection of the region in 10×10 in sky view virtual observatory: The parameters used during sky survey are listed below: Coordinate: J2000, Projection: Gnomonic Image size (pixel): 500×500 Brightness scaling: Histogram Equalization Step-II: Image taken on the basis of searching isolated cavity structure around AGB star Step-III: Extraction of flux using Aladin v2.503 software(https://aladin.u-strasbg.fr/aladin.gml): The Flexible Image Transport System (FITS) images were downloaded from sky view, according to the procedure mentioned above and the FITS image is processed using software Aladin v2.503. Region of interest The image structure located at R.A. (J2000) = 04hr 46m33.036s and Dec. (J2000) = +490 56m 23.77s selected as a region of our interest. The reasons of selections are as follows: 1 The structure seems to be isolated and its size is around 3.24 pc for IRIS and 12.28 pc for AKARI in contraction. 2 There were several condensations (minima) and the features can be seen in all 4 bands of IRIS survey and AKARI survey. 3 The structure in IRIS is prominent in 60µm and 100µm that enable us to study the fluxes emitted from the dust and grain. 4 The structure in AKARI is prominent in 90µm (AKARI WIDE-S) and 140µm (AKARI WIDE-L) that enable us to study the fluxes emitted from the dust and grain. Data reduction Each pixel of the cavity-like region in FITS images are analyzed by using Aladin v2.503 which helps in data reduction. With the help of Aladin v2.503 the invisible spectral photography can be reduced into desired color and analysis of the relative flux distribution in the region of interest can be done. More precisely we cannot make visible pictures and photography in IR region but, using this software we can make visible reference with color specification. So it is convenient to draw contour map, hexbin plot and marking to find desired physical parameter (e.g. Flux, coordinate, etc). The Aladin software can be considered as sky ATLAS designed by CDS for research of astronomical sources through color coded display of required http://web.chungbuk.ac.kr/~kwsuh/agb.htm Devendra Raj Upadhyay and Trishna Subedi/BIBECHANA 18 (2) (2021) 154-163 156 image. Aladin v2.503 allows us to visualize digitized images of any part of the sky, to superimpose entries from the CDS astronomical catalogs and tables, and to interactively access related data and information from SIMBAD and Gaia Archive of all known objects in the field. Flux density variation We studied the flux density of all the pixel lying inside the counter level 71 for IRIS under 100µm and find the flux of corresponding pixels in 60µm using the software Aladin v2.503 which was used to calculate the dust color temperature and mass of each pixel due to the contribution of dust. Similarly, for AKARI we used the counter level 100 under 140 µm image and the corresponding pixels in 90 µm were obtained. Here we found the regions of maximum and minimum flux and studied the density in each image of both IRIS and AKARI in a comparative manner. Dust color temperature The contour map has been made in 100 m and 140 m FITS. Then the corresponding flux densities are calculated from the IRIS 60 µm image. Using the ratio of the flux density in the IRIS 60 µm to the flux density in the IRIS 100 µm in the expression given below [20, 21] , dust color temperature is calculated as, �� = −96 ln �×0.643+� ….… (1) where, � = � 60�� � 100�� Since, F (60µm) and F (100µm) are the flux densities at 60µm and 100µm respectively. For AKARI survey, following expression is used to calculate the dust color temperature [6, 20, 21], �� = −57 ln �×0.643+� ...… (2) where, � = � 90�� � 140�� Since, F (90µm) and F (140µm) are the flux densities at 90µm and 140µm respectively. Dust mass estimation The dust masses are estimated from the far-infrared flux densities at 100 μm image in IRIS and 140 μ m in AKARI survey. The infrared flux can be measured from the IRIS sky view images and images from Groningen using Aladin v2.503. The resulting dust mass depends on the physical and chemical properties of the dust grains, the adopted dust temperature and the distance to the object. The final expression for the dust mass [22-24], can be written as; �dust = 4aρ 3�� ���2 � �,� ..… (3) Here, B(v,T) = Planck’s function, which is the function of the temperature and frequency, and given by the expression; � �, � = 2ℎ�3 �2 1 � ℎ� KT−1 .….. (4) and a= Weighted grain size = 0.1 μm ρ = Grain density= 3000 kgm-3 Qν= grain emissivity = 0 .0010 for 100μm and 0.0046 for 60μm respectively. Fν= total flux density of the region whose mass is to be determined, �� = � × 5.288 × 10−9 MJysr-1 1MJysr-1=1.26×10–19kg.s–2 D = distance to the structure B(ν,T) = Planck’s function. h = Planck’s constant c = velocity of light ν = frequency at which the emission is observed and T= the average temperatures of the region. Values of different parameters we use in the calculation of the dust mass in our interest are as follows: Using these values, an expression (3) takes the form [22-24], �dust = 0.40 ���2 � �,� ....… (5) Visual extinction For visual extinction we need optical depth[25] �100 = �100µ� � �,� 100 …… (6) Here F100µm in kgs-2 and B(ν,T)100 is corresponding intensity of radiation which is observed at 100 µm h Devendra Raj Upadhyay and Trishna Subedi/BIBECHANA 18 (2) (2021) 154-163 157 flux in IRIS as proposed by Wood et al. [14]. For visual extinction: �� = 15.078 1 − � −�100 641.3 …… (7) We have uses this formula for AKARI by calculating optical depth for τ140. For AKARI survey, following expression is used to calculate the visual extinction �� = 15.078 1 − � −�140 641.3 ..…… (8) where �140 = �140µ� � �,� 140 Inclination angle The angle between line-of-sight and the plane of celestial object projected in the sphere is called inclination angle. Holmberg (1946) [26] established a simple model to find the inclination angle of celestial objects. Holmberg equation is the relation between the axial ratio ( b/a ) and the inclination angle (i), the angle between the line-of-sight and normal to the galactic plane. The flatness factor (q) = 0.33 is assumed by considering oblate spheroid. ���2� = �2 �2 −�2 �2 ……..(9) is called ‘Holmberg Formula’ for inclination angle [26]. 3. Results and Discussion In our work, the dust color temperature, intensity of radiation, dust mass and extension are measured using FITS images of 60 μm, 100 μm and 90 μm, 140 μm. Projection map of coordinates in R. A. and DECL Fig. 1 is the projection map of the right accession and declination. It show larger region of interest in Fig. 1(a) IRIS in comparison with Fig. 1(b) because we have selected image size 10×10 for IRIS and 0.50×0.50 in AKARI. But we obtained more pixels in AKARI because of high resolution of survey. This projection is lambert projection in nature. Fig. 1: Position of candidate IRAS 04427+4951 (a) Projection of coordinates of far infrared cavities using IRIS survey (b) Projection that of coordinates using data of AKARI survey. Hexbin distributions of flux Fig. 2 (a) show the 60 micrometer IRIS image flux distribution in MJysr-1 with R.A.(J2000) and DECL.(J2000) in degree in IRIS survey. Similarly, Fig. 2 (b) show the 90 micrometer AKARI FITS image flux distribution in MJysr-1 with R.A.(J2000) and DECL.(J2000) in degree in IRIS survey. Here, color ranging from violet to red indicates more emission of flux from that pixels. In both case the central region contain lesser flux in low wavelength band of both survey. Devendra Raj Upadhyay and Trishna Subedi/BIBECHANA 18 (2) (2021) 154-163 158 Fig. 2: (a) represents hexbin plot of right ascension (R.A.), declination (DECL.) and 60 m flux using IRIS survey (b) hexbin plot of right ascension (R.A.), declination (DECL.) and 90 m flux of IRAS 04427+4951 using AKARI survey. Mapping of flux Fig. 3 (a) present the contour map of 100 micrometer IRIS FITS image flux distribution in MJysr-1 with R.A.(J2000) and DECL. (J2000) in degree in IRIS survey. Similarly, Fig. 3(b) show the 140 micrometer AKARI FITS image flux distribution in MJysr-1with R.A.(J2000) and DECL.(J2000) in degree. Here, color bar ranging from red to violet indicate decrease in flux which show the cavity region of asymptotic giant branch at center in both survey. Fig. 3: The contours are shown. (a) 100 μm flux (b) 140 μ m flux with right ascension (R.A.), declination (DECL.) using AKARI survey. Linear fit of Flux Fig. 4(a) represents the best fit between the far- infrared flux of 60 μm and 100 μm. Similarly, Fig. 4(b) shows the best fit relation between far-infrared flux emission in 90 μm and 140 μm. Here, the data extracted from the FITS image of the IRIS and AKARI survey. Devendra Raj Upadhyay and Trishna Subedi/BIBECHANA 18 (2) (2021) 154-163 159 Fig. 4: (a) Linear fit between flux of 60 μm and 100 μm (b) Linear fit between flux 90 μm and 140 μm. Both has positive slope. The best fit line obtained are: F60=0.28F100 - 1.16 ……..(10) F90=0.10F140 + 7.33 ……..(11) Here, F60, F100, F90 and F140 are flux in MJysr-1. The slope of these line are 0.28 and 0.10 used for the calculation of dust color temperature. The coefficient of correlation 0.85 in IRIS data and 0.53 in AKARI data which shows flux at central region of infrared cavity are more diverse. Mapping of dust color temperature Fig. 5 presents the contour map of dust color temperature distribution. Here, color means the temperature depends upon the wavelength of radiation emitted by a cloud of dust from the cavity region around AGB stars. Fig. 5: represents contour map of dust color temperature (a) using IRIS data. (b) using AKARI survey. The contour and color bar distinguish the color temperature of radiation. On comparing two survey data, the dust color temperature is more in IRIS whereas lesser in AKARI. It shows higher the wavelength band lesser the temperature. From this study, the dust color temperature is in the range between 22.85 K and 24.1 K with an average dust color temperature of 23.48 K in the IRIS survey and 14.54 K to 15.24 K with an average dust color temperature of 14.89 K in the AKARI survey. Mapping of Planck’s function Fig. 6 shows intensity of radiation distributions in far-infrared radiation emitted by a cloud of dust around AGB stars corresponding to dust color temperature. Devendra Raj Upadhyay and Trishna Subedi/BIBECHANA 18 (2) (2021) 154-163 160 Fig. 6: Contour map of Planck's function (a) using IRIS data. (b) using AKARI survey. The contours and color separate the different intensities of radiation. In the given Fig. 6(a) and (b), the color bar represents the radiation intensity increases from violet to red. Looking at the iso- contours we generated, the IRIS plot shows the spectral intensity decrement towards the center, but the maximum intensity lies a little away from the center. However, the AKARI plot shows the irregular trends in Planck's function values. Here, different in trend due to polytropy nature of the dust in the region around AGB stars. Mapping of dust mass Fig. 7 present the contour map of dust mass in the cavity created due to AGB wind. By calculation we obtained the average dust mass is 3.55 × 1027 kg (1.79 ×10-3Mʘ) using IRIS FITS observation and 5.34×1028 kg (2.69 × 10-2 Mʘ ) in AKARI FITS analysis. Here on comparing from Fig. 5, Fig. 6, and Fig. 7 in both survey dust mass is more in that region where dust color temperature and Planck's function minimum. It shows a nearly inverse trend of dust mass with the dust color temperature, Planck's function. Fig. 7: Contour map of dust mass using ( a) IRIS data. (b) contour map using AKARI survey. Visual Extinction Fig. 8 (a) and (b) show the variation of dust color temperature with visual extinction in both surveys. The values are in the range of 4.3 × 10-4 - 3.4 × 10-4 mag in IRIS and 7.5 × 10-3 - 4.5 × 10-3 mag in AKARI. Here, temperature has inverse relation with visual extinction in both survey. The best fit line for IRIS and AKARI data obtained are: Devendra Raj Upadhyay and Trishna Subedi/BIBECHANA 18 (2) (2021) 154-163 161 Td=-0.75Av +26.12 ……..(12) Td=-0.23Av + 16.16 ……..(13) The coefficient of correlation are -0.72 in IRIS data and -0.96 in AKARI data. This show that AKARI survey is more intensive and more responsive. Fig. 8: The variation of dust color temperature (Td ) with visual extinction ( AV ) (a) for IRIS and (b) for AKARI survey. Table 1: Structure of the cavity in terms of extension contraction and inclination angle. Table 1 shows the extension (major diameter) contraction(minor diameter), inclination angle values. Here, the size of the cavity region we have selected in IRIS is more (36.56×12.28) pc whereas structure is small in AKARI image (10.02×3.24) pc since we have taken 10×10 size in IRIS and 0.50× 0.50. Extension and contraction of the structure obtained using a simple expression L = R × θ, where R = 3000.36 pc is the distance to the structure and θ = pixel length (in radian). The value of inclination angle is nearly 900 shows cavity structure suggesting an edge-on appearance. 4. Conclusions We have studied physical properties (flux variation, dust color temperature, dust mass estimation, distance, Planck’s function, and extinction) of the cavity region around structure IRAS 04427+4951 within 10×10 for IRIS all-sky map and 0.50×0.50 for AKARI all-sky map. We focus on the dust environment of AGB stars. The search of the dust structure in far-infrared (100 µm and 60 µm) of various AGB stars in IRIS database and (140 µm and 90 µm) in AKARI all-sky map perform. The distance to the AGB star is 3000.36 pc. The size of cavity-like structure around AGB star in IRIS all sky map is found to be 36.56 pc×12.28 pc and AKARI all sky map is found to be 10.02 pc×3.24 pc. The difference in the obtained size is found due to different size during target extraction i.e., 1⁰×1⁰ for IRIS all sky map and 0.5⁰× 0.5⁰ for AKARI all sky map and also due to the independent contour map drawn for different map. From the IRIS and AKARI map, we have seen the minimum flux region is at the center of the cavity. The Physical properties of a cavity of our region of interest are studied. We have extensively used the help of Aladin v2.5 and Python 3. We tagged each pixel and the data of flux density extracted and dust color temperature, dust mass estimation, size of the structure, inclination angle, and visual extinction. From the above study, we obtain the dust color temperature in the range between 22.85K and 24.1 K with an average dust color temperature of 23.48 K in the Source Extension Contraction Inclination angle IRIS 36.56 12.28 86.150 AKARI 10.02 3.24 86.080 Devendra Raj Upadhyay and Trishna Subedi/BIBECHANA 18 (2) (2021) 154-163 162 IRIS survey and 14.54K -15.24K with an average dust color temperature of 14.89K in the AKARI survey. The average dust mass is 3.55 × 1027 kg (1.79 ×10-3Mʘ) in IRIS survey and 5.34×1028 kg (2.69 × 10-2 Mʘ )in AKARI survey. The dust color temperature and dust mass show a nearly inverse relation with each other which supports our physics. The average value of spectral density is 8.75 × 10-16 Wm-2sr-1Hz-1 and 1.47 10-16 Wm-2sr-1Hz-1 using FITS of IRIS and AKARI The size of the structure is found to be 36.56pc × 12.28 pc with inclination angle 86.150 in IRIS and 10.02 pc × 3.24 pc with inclination angle 86.08 0 in AKARI map. The visual extinction is found to be in the range of 4.3 × 10-4 - 3.4 × 10-4 mag in IRIS and 7.5 × 10-3 - 4.5 × 10-3 mag in AKARI. On comparing past dust properties obtain using IRIS and AKARI and our results. Here, we reach an understanding of lesser dust color temperature, more mass, and extension. It supports the structure such as polyaromatic hydrocarbon, graphene, etc. formation process in the interstellar medium. The dust properties around C-rich, O-rich, S-rich, and Si-rich will do using the spitzer, 2Mass, and WISE survey. 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