Zobrazeno 1 - 10
of 1 863
pro vyhledávání: '"SHARMA, SAURABH"'
Autor:
Verma, Aayushi, Sharma, Saurabh, Dewangan, Lokesh K., Ojha, Devendra K., Mallick, Kshitiz, Yadav, Ram Kesh, Kaur, Harmeen, Chand, Tarak, Agarwal, Mamta, Gupta, Archana
We aim to investigate the global star formation scenario in star-forming sites AFGL 5157, [FSR2007] 0807 (hereafter FSR0807), [HKS2019] E70 (hereafter E70), [KPS2012] MWSC 0620 (hereafter KPS0620), and IRAS 05331+3115 in the outer galactic arm. The d
Externí odkaz:
http://arxiv.org/abs/2406.10388
Autor:
Sharma, Saurabh, Borissova, Jura
Red giants are an excellent tool for probing the history of star formation and subsequent metallicity evolution in the galaxies. The well-defined red giant branch (RGB) stars of the globular clusters can be used to determine their slopes and to calib
Externí odkaz:
http://arxiv.org/abs/2406.09911
Autor:
Panwar, Neelam, C., Rishi, Sharma, Saurabh, Ojha, Devendra K., Samal, Manash R., Singh, H. P., Yadav, Ram Kesh
We present a multi-wavelength analysis of the young star cluster Berkeley 59 (Be 59) based on the $Gaia$ data and deep infrared (IR) observations with the 3.58-m Telescopio Nazionale Galileo and $Spitzer$ space telescope. The mean proper motion of th
Externí odkaz:
http://arxiv.org/abs/2406.08261
We have carried out a quantitative analysis of the $1^{\circ} \times 1^{\circ}$ region near star-forming site AFGL 5157 using 'Minimal Spanning Tree' (MST). The analysis reveals that this region consists of five major clusters. The cluster radii of t
Externí odkaz:
http://arxiv.org/abs/2404.13935
Autor:
Ghosh, Arpan, Sharma, Saurabh, Ninan, Joe Philip, Ojha, Devendra K., Verma, Aayushi, Sahu, Tarak Chand, Pandey, Rakesh, Singh, Koshvendra
We present here initial results of our spectro-photometric monitoring of XZ Tau. During our monitoring period, XZ Tau exhibited several episodes of brightness variations in timescales of months at optical wavelengths in contrast to the mid-infrared w
Externí odkaz:
http://arxiv.org/abs/2404.09361
Autor:
Singh, Koshvendra, Ninan, Joe P., Romanova, Marina M., Buckley, David A. H., Ojha, Devendra K., Ghosh, Arpan, Monson, Andrew, Schramm, Malte, Sharma, Saurabh, Reichart, Daniel E., Mikolajewska, Joanna, Beamin, Juan Carlos, Borissova, J., Ivanov, Valentin D., Kouprianov, Vladimir V., Hambsch, Franz-Josef, Pearce, Andrew
EX Lupi, a low-mass young stellar object, went into an accretion-driven outburst in March of 2022. The outburst caused a sudden phase change of ~ 112$^{\circ}$ $\pm$ 5$^{\circ}$ in periodically oscillating multiband lightcurves. Our high resolution s
Externí odkaz:
http://arxiv.org/abs/2404.05420
Recent surveys have demonstrated the widespread presence of UV emission in early-type galaxies (ETGs), suggesting the existence of star formation in many of these systems. However, potential UV contributions from old and young stars, together with mo
Externí odkaz:
http://arxiv.org/abs/2403.12160
Autor:
Sharma, Saurabh, SIngh, Ambuj
The problem of online social network manipulation for community canvassing is of real concern in today's world. Motivated by the study of voter models, opinion and polarization dynamics on networks, we model community canvassing as a dynamic process
Externí odkaz:
http://arxiv.org/abs/2403.12399
Autor:
Dewangan, L. K., Jadhav, O. R., Maity, A. K., Bhadari, N. K., Sharma, Saurabh, Padovani, M., Baug, T., Mayya, Y. D., Pandey, Rakesh
To probe the star formation process, we present an observational investigation of the Pillar IV and an ionized knot HH 216 in the Eagle Nebula (M16). Pillar IV is known to host a Class I protostar that drives a bipolar outflow. The outflow has produc
Externí odkaz:
http://arxiv.org/abs/2401.06016
Autor:
Sharma, Saurabh, Verma, Aayushi, Mallick, Kshitiz, Dewangan, Lokesh K., Kaur, Harmeen, Yadav, Ram Kesh, Panwar, Neelam, Ojha, Devendra K., Chand, Tarak, Agarwal, Mamta
We present a multi-wavelength analysis of the star cluster NGC 2316 and its surroundings. We estimated the physical parameters of the NGC 2316 cluster, including its shape (elongated), size (Rcluster = 0.4 pc), distance (1.3 +/- 0.3 kpc), and minimum
Externí odkaz:
http://arxiv.org/abs/2312.17699