Design and development of Mt.Abu faint object spectrograph and camera – Pathfinder (MFOSC-P) for PRL 1.2m Mt. Abu Telescope

Srivastava, Mudit; Kumar, Vipin; Dixit, Vaibhav; Patel, Ankita; Jangra, Mohanlal; Rajpurohit, A. S.; Mathur, Satya N.

doi:10.1007/s10686-021-09753-5

Cited by 7 publications

(2 citation statements)

References 27 publications

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“…As part of the ongoing project, we had optical observations of the system at a few epochs before it went into the X-ray outburst. We continued our optical spectroscopic observations of 1A 0535+262 during the X-ray outburst using the 1.2 m telescope of the Mount Abu Infrared Observatory with the Faint Object Spectrograph and Camera-Pathfinder (MFOSC-P) instrument (Srivastava et al 2018;Srivastava et al 2021) mounted on the 1.2 m, f/13 telescope at several epochs. The instrument is designed to provide seeing limited imaging in Bessel BVRI filters with a sampling rate of 3.3 pixels per arc-second over a 5.2×5.2 arc-minute 2 field-of-view.…”

Section: Optical Observationsmentioning

confidence: 99%

Optical and X-ray studies of Be/X-ray binary 1A 0535+262 during its 2020 giant outburst

Chhotaray

Jaisawal

Kumari

et al. 2022

Monthly Notices of the Royal Astronomical Society

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We report results obtained from the optical and X-ray studies of the Be/X-ray binary 1A 0535+262/HD 245770 during the 2020 October giant X-ray outburst, using the 1.2 m telescope at Mount Abu Infrared observatory and AstroSat, respectively. The peak flux of the outburst was recorded to be ∼11 Crab in the 15–50 keV range, the highest ever observed from the pulsar. We performed optical observations in the 6000–7200 Å band before, during, and after the outburst to investigate the evolution of the circumstellar disc of the Be star between 2020 February and 2022 February. Our optical spectra exhibit prominent emission lines at 6563 Å (H i), 6678 Å (He i), and 7065 Å (He i). We found a significantly variable Hα line in the spectra. The single-peaked line profile appeared asymmetric with broad red- & blue-wings in the data before and during the outburst. The post-outburst observations, however, resulted in a double-peaked profile with asymmetry in the blue-wing. Our observations before the outburst confirmed a larger Be disc that decreased in size as the outburst progressed. Furthermore, the observed variabilities in the Hα line profile and parameters suggest the presence of a highly misaligned, precessing, and warped Be disc. AstroSat observation of the pulsar detected pulsations at ∼103.55 s in the light curve up to 110 keV. We found strongly energy-dependent pulse profiles with increasing contribution of the pulsing component in hard X-rays. The broadband spectral fitting in the 0.7-90.0 keV range confirmed the presence of the known cyclotron resonance scattering feature at ∼46.3 keV.

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Section: Optical Observationsmentioning

confidence: 99%

Optical and X-ray studies of Be/X-ray binary 1A 0535+262 during its 2020 giant outburst

Chhotaray

Jaisawal

Kumari

et al. 2022

Monthly Notices of the Royal Astronomical Society

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“…Optical photometry and spectroscopy of V2891 Cyg were carried out with the Mount-Abu Faint Object Spectrograph and Camera-Pathfinder (MFOSC-P) instrument on the 1.2 m Mount Abu telescope (Srivastava et al 2018;Rajpurohit et al 2020;Srivastava et al 2021). The instrument provides seeing-limited imaging in the Bessell 𝐵𝑉𝑅𝐼 filters over a 5.2 × 5.2 arc-minute 2 field of view, with a sampling of 3.3 pixels per arc-second.…”

Section: Optical Observations From Mt Abumentioning

confidence: 99%

Optical and near-infrared spectroscopy of Nova V2891 Cygni: evidence for shock-induced dust formation

Kumar¹,

Srivastava

Banerjee

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We present multi-epoch optical and near-infrared observations of the highly reddened, Fe ii class slow nova V2891 Cygni. The observations span 15 months since its discovery. The initial rapid brightening from quiescence, and the presence of a ∼35 day long pre-maximum halt, is well documented. The evidence that the current outburst of V2891 Cyg has undergone several distinct episodes of mass ejection is seen through time-varying P Cygni profiles of the O i 7773 Å line. A highlight is the occurrence of a dust formation event centred around ∼+273d, which coincides with a phase of coronal line emission. The dust mass is found to be ∼0.83 − 1.25 × 10−10 M⊙. There is strong evidence to suggest that the coronal lines are created by shock heating rather than by photoionization. The simultaneous occurrence of the dust and coronal lines (with varying velocity shifts) supports the possibility that dust formation is shock-induced. Such a route for dust formation has not previously been seen in a nova, although the mechanism has been proposed for dust formation in some core-collapse supernovae. Analysis of the coronal lines indicates a gas mass and temperature of 8.35–8.42 × 10−7 M⊙ and ∼(4.8 − 9.1) × 105 K respectively, and an overabundance of aluminium and silicon. A Case B analysis of the hydrogen lines yields a mass of the ionized gas of (8.60 ± 1.73) × 10−5 M⊙. The reddening and distance to the nova are estimated to be E(B − V) = 2.21 ± 0.15 and d = 5.50 kpc respectively.

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A summary of instruments proposed for observing pulsating variables from the Mt. Abu Observatory

Mishra,

Sarkar,

Prajapati

et al. 2024

J Astrophys Astron

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Design and development of Mt.Abu faint object spectrograph and camera – Pathfinder (MFOSC-P) for PRL 1.2m Mt. Abu Telescope

Cited by 7 publications

References 27 publications

Optical and X-ray studies of Be/X-ray binary 1A 0535+262 during its 2020 giant outburst

Optical and X-ray studies of Be/X-ray binary 1A 0535+262 during its 2020 giant outburst

Optical and near-infrared spectroscopy of Nova V2891 Cygni: evidence for shock-induced dust formation

A summary of instruments proposed for observing pulsating variables from the Mt. Abu Observatory

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