UVIT study of UV bright stars in the globular cluster NGC 4147

Kumar, Ranjan; Pradhan, Ananta C.; Parthasarathy, M.; Ojha, D. K.; Mohapatra, Abhisek; Murthy, Jayant; Cassisi, S.

doi:10.1007/s12036-020-09687-y

Cited by 6 publications

(4 citation statements)

References 48 publications

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“…Optical identification of AstroSat discovered sources was one of the prime goals of the 3.6-m DOT and the 4K×4K CCD Imager (Sagar 2018, Pandey et al2018. Recently, Kumar et al (2021) identified several AstroSat-UVIT sources in the field of NGC 4147. These objects are located in different stages of stellar evolution in the UV-optical CMDs showing properties of blue horizontal branch stars, blue straggler star and variable stars.…”

Section: The Colour-magnitude Diagram Of Ngc 4147mentioning

confidence: 99%

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Optical Observations of star clusters NGC 1513 and NGC 4147; white dwarf WD1145+017 and $K$ band imaging of star forming region Sh2-61 with the 3.6 meter Devasthal Optical Telescope

Sagar,

Yadav,

Pandey

et al. 2022

Preprint

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The U BVRI CCD photometric data of open star cluster NGC 1513 are obtained with the 3.6-m Indo-Belgian Devasthal optical telescope (DOT). Analyses of the GAIA EDR3 astrometric data have identified 106 possible cluster members. The mean proper motion of the cluster is estimated as µ α Cosδ = 1.29 ± 0.02 and µ δ = −3.74 ± 0.02 mas yr −1 . Estimated values of reddening E(B − V) and distance to the NGC 1513 are 0.65±0.03 mag and 1.33±0.1 kpc respectively. An age of 225 ± 25 Myr is assigned to the cluster by comparing theoretical isochrones with deep observed cluster sequence. Using observations taken with the 3.6-m DOT, values of distance and age of the galactic globular cluster NGC 4147 are estimated as 18.2 ± 0.2 Kpc and 14 ± 2 Gyr respectively. The optical observations of planetary transit around white dwarf WD1145+017 and K-band imaging of star-forming region Sharpless Sh 2-61 demonstrate observing capability of 3.6-m DOT. Optical and near-infrared observations of celestial objects and events are being carried out routinely with the 3.6-m DOT. They indicate that the performance of the telescope is at par with those of other similar telescopes located elsewhere in the world. We therefore state that this observing facility augurs well for multi-wavelength astronomy including study of astrophysical jets.

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Section: The Colour-magnitude Diagram Of Ngc 4147mentioning

confidence: 99%

“…While Lata et al (2019) have discovered several different types of variables within core region of the NGC 4147 using optical observations taken with the 4K×4K CCD imager 2 by Lata et al (2019). It is numbered as HB24 in Table 4 of Kumar R. et al (2021).…”

Section: The Colour-magnitude Diagram Of Ngc 4147mentioning

confidence: 99%

Optical Observations of star clusters NGC 1513 and NGC 4147; white dwarf WD1145+017 and $K$ band imaging of star forming region Sh2-61 with the 3.6 meter Devasthal Optical Telescope

Sagar,

Yadav,

Pandey

et al. 2022

Preprint

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“…However, depending upon the environment during merger or collision, the mass and age of BSs are slightly different from single star evolution (Sills et al 2009;Sun et al 2021). Due to their extremely large effective temperature, a UV imaging study is a powerful tool to identify and trace the properties of BSs in GCs (Ferraro 2000;Raso et al 2017;Ferraro et al 2018;Sindhu et al 2019;Sahu et al 2019a;Subramaniam et al 2020;Kumar et al 2021a).…”

mentioning

confidence: 99%

“…The physical parameters such as (T eff ), radius, luminosity, mass, etc., have been derived for the UV bright sources of various evolutionary stages (EHBs, BHBs, BSs, etc.) using UVIT and other available optical photometric observations (Sahu et al 2019a;Singh et al 2020;Kumar et al 2020Kumar et al , 2021aPrabhu et al 2021;Rani et al 2021). The stellar evolutionary models such as BaSTI (old) and BaSTI-IAC (updated) (Pietrinferni et al 2004;Hidalgo et al 2018;Pietrinferni et al 2021), FSPS models (Conroy et al 2009), Padova isochrone sets (Marigo & Girardi 2007), Y 2 stellar evolutionary tracks (Lee et al 2015), etc., have well incorporated in deriving these parameters.…”

mentioning

confidence: 99%

Study of UV bright sources in globular cluster NGC 4590 using Ultraviolet Imaging Telescope (UVIT) observations

Kumar,

Pradhan,

Parthasarathy

et al. 2022

Preprint

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We have studied ultraviolet (UV) bright sources in the Galactic globular cluster (GGC) NGC 4590 using Ultraviolet Imaging Telescope (UVIT) on-board the AstroSat satellite. Using UVoptical color-magnitude diagrams (CMDs), we have identified and characterized the sources of different evolutionary stages i.e., blue horizontal branch stars (BHBs), extremely blue horizontal branch stars (EHBs), blue straggler stars (BSs), variable stars, etc. We estimated effective temperature (T eff ), gravity (log(g)), luminosity (L bol ), and hence the radius (R) of these hot stars by fitting spectral energy distribution (SED) with the help of stellar atmosphere models. Two new far-UV (FUV) bright cluster member stars situated near the core of the cluster have been detected; one of them is an EHB star and the other one is either in its post-blue hook evolutionary phase or in white dwarf phase. The evolutionary status of all the hot stars, identified in the cluster, has been investigated by using various evolutionary models. We find the massive and younger BSs are concentrated at the center of the cluster whereas the older and less massive BSs are distributed though out the cluster. The BSs normalized radial distribution seems to be bi-modal with a minimum located at r min = 4.3 r c . We calculated A + parameter of the cluster which is obtained using cumulative normalized radial distribution of horizontal branch stars (HBs) and BSs. We measured this value up to half-mass radius of the cluster to be +0.13, which indicates that NGC 4590 is one of the youngest clusters among dynamically intermediate age GGCs with a dynamical age of 0.423 ± 0.096 Gyr.

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Optical observations of star clusters NGC 1513 and NGC 4147; white dwarf WD 1145$$+$$017 and K band imaging of star-forming region Sh 2-61 with the 3.6-m Devasthal optical telescope

et al. 2022

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UVIT study of UV bright stars in the globular cluster NGC 4147

Cited by 6 publications

References 48 publications

Optical Observations of star clusters NGC 1513 and NGC 4147; white dwarf WD1145+017 and $K$ band imaging of star forming region Sh2-61 with the 3.6 meter Devasthal Optical Telescope

Optical Observations of star clusters NGC 1513 and NGC 4147; white dwarf WD1145+017 and $K$ band imaging of star forming region Sh2-61 with the 3.6 meter Devasthal Optical Telescope

Study of UV bright sources in globular cluster NGC 4590 using Ultraviolet Imaging Telescope (UVIT) observations

Optical observations of star clusters NGC 1513 and NGC 4147; white dwarf WD 1145$$+$$017 and K band imaging of star-forming region Sh 2-61 with the 3.6-m Devasthal optical telescope

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