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Your search keyword '"Singh, Mridweeka"' showing total 4 results
Start Over Author "Singh, Mridweeka" Publisher stockholms universitet, institutionen for astronomi
4 results on '"Singh, Mridweeka"'

1. The Fast-evolving Type Ib Supernova SN 2015dj in NGC 7371

Author

Singh, Mridweeka, Misra, Kuntal, Valenti, Stefano, Hosseinzadeh, Griffin, Pastorello, Andrea, Srivastav, Shubham, Gangopadhyay, Anjasha, Dastidar, Raya, Tomasella, Lina, Arcavi, Iair, Benetti, Stefano, Callis, Emma, Cappellaro, Enrico, Elias-Rosa, Nancy, Howell, D. Andrew, Kim, Sang Chul, McCully, Curtis, Tartaglia, Leonardo, Terreran, Giacomo, Turatto, Massimo, Singh, Mridweeka, Misra, Kuntal, Valenti, Stefano, Hosseinzadeh, Griffin, Pastorello, Andrea, Srivastav, Shubham, Gangopadhyay, Anjasha, Dastidar, Raya, Tomasella, Lina, Arcavi, Iair, Benetti, Stefano, Callis, Emma, Cappellaro, Enrico, Elias-Rosa, Nancy, Howell, D. Andrew, Kim, Sang Chul, McCully, Curtis, Tartaglia, Leonardo, Terreran, Giacomo, and Turatto, Massimo

Abstract

We present the detailed optical evolution of a Type Ib SN 2015dj in NGC 7371, using data spanning up to similar to 170 days after discovery. SN 2015dj shares similarity in light-curve shape with SN 2007gr and peaks at M-V = -17.37 +/- 0.02 mag. Analytical modeling of the quasi bolometric light curve yields 0.06 +/- 0.01 M-circle dot of Ni-56, ejecta mass = M-ej = 1.4(-0.5)(+1.3) M-circle dot, and kinetic energy E-k = 0.7(-0.3)(+0.6) x 10(51) erg. The spectral features show a fast evolution and resemble those of spherically symmetric ejecta. The analysis of nebular phase spectral lines indicates a progenitor mass between 13-20 M-circle dot, suggesting a binary scenario.

Published
2021
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2. Optical studies of two stripped-envelope supernovae – SN 2015ap (Type Ib) and SN 2016P (Type Ic)

Author

Gangopadhyay, Anjasha, Misra, Kuntal, Sahu, D. K., Wang, Shan-Qin, Kumar, Brajesh, Li, Long, Anupama, G. C., Dastidar, Raya, Elias-Rosa, N., Kumar, Brijesh, Singh, Mridweeka, Pandey, S. B., Sanwal, Pankaj, Singh, Avinash, Srivastav, S., Tartaglia, Leonardo, Tomasella, L., Gangopadhyay, Anjasha, Misra, Kuntal, Sahu, D. K., Wang, Shan-Qin, Kumar, Brajesh, Li, Long, Anupama, G. C., Dastidar, Raya, Elias-Rosa, N., Kumar, Brijesh, Singh, Mridweeka, Pandey, S. B., Sanwal, Pankaj, Singh, Avinash, Srivastav, S., Tartaglia, Leonardo, and Tomasella, L.

Abstract

We present the photometric and spectroscopic studies of a Type Ib SN 2015ap and a Type Ic SN 2016P. SN 2015ap is one of the bright (MV = −18.04 mag) Type Ib while SN 2016P lies at an average value among the Type Ic SNe (MV = −17.53 mag). Bolometric light-curve modelling of SNe 2015ap and 2016P indicates that both the SNe are powered by 56Ni + magnetar model with 56Ni masses of 0.01 and 0.002 M⊙, ejecta masses of 3.75 and 4.66 M⊙, spin period P0 of 25.8 and 36.5 ms, and magnetic field Bp of 28.39 × 1014 and 35.3 × 1014 G, respectively. The early spectra of SN 2015ap show prominent lines of He with a ‘W’ feature due to Fe complexes while other lines of Mg ii, Na i, and Si ii are present in both SNe 2015ap and 2016P. Nebular phase [O i] profile indicates an asymmetric profile in SN 2015ap. The [O i]/[Ca ii] ratio and nebular spectral modelling of SN 2015ap hint towards a progenitor mass between 12 and 20 M⊙.

Published
2020
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3. SN 2017gmr : An Energetic Type II-P Supernova with Asymmetries

Author

Andrews, Jennifer E., Sand, D. J., Valenti, S., Smith, Nathan, Dastidar, Raya, Sahu, D. K., Misra, Kuntal, Singh, Avinash, Hiramatsu, D., Brown, P. J., Hosseinzadeh, G., Wyatt, S., Vinko, J., Anupama, G. C., Arcavi, I., Ashall, Chris, Benetti, S., Berton, Marco, Bostroem, K. A., Bulla, Mattia, Burke, J., Chen, S., Chomiuk, L., Cikota, A., Congiu, E., Cseh, B., Davis, Scott, Elias-Rosa, N., Faran, T., Fraser, Morgan, Galbany, L., Gall, C., Gal-Yam, A., Gangopadhyay, Anjasha, Gromadzki, M., Haislip, J., Howell, D. A., Hsiao, E. Y., Inserra, C., Kankare, E., Kuncarayakti, H., Kouprianov, V., Kumar, Brajesh, Li, Xue, Lin, Han, Maguire, K., Mazzali, P., McCully, C., Milne, P., Mo, Jun, Morrell, N., Nicholl, M., Ochner, P., Olivares, F., Pastorello, A., Patat, F., Phillips, M., Pignata, G., Prentice, S., Reguitti, A., Reichart, D. E., Rodriguez, O., Rui, Liming, Sanwal, Pankaj, Sarneczky, K., Shahbandeh, M., Singh, Mridweeka, Smartt, S., Strader, J., Stritzinger, M. D., Szakats, R., Tartaglia, Leonardo, Wang, Huijuan, Wang, Lingzhi, Wang, Xiaofeng, Wheeler, J. C., Xiang, Danfeng, Yaron, O., Young, D. R., Zhang, Junbo, Andrews, Jennifer E., Sand, D. J., Valenti, S., Smith, Nathan, Dastidar, Raya, Sahu, D. K., Misra, Kuntal, Singh, Avinash, Hiramatsu, D., Brown, P. J., Hosseinzadeh, G., Wyatt, S., Vinko, J., Anupama, G. C., Arcavi, I., Ashall, Chris, Benetti, S., Berton, Marco, Bostroem, K. A., Bulla, Mattia, Burke, J., Chen, S., Chomiuk, L., Cikota, A., Congiu, E., Cseh, B., Davis, Scott, Elias-Rosa, N., Faran, T., Fraser, Morgan, Galbany, L., Gall, C., Gal-Yam, A., Gangopadhyay, Anjasha, Gromadzki, M., Haislip, J., Howell, D. A., Hsiao, E. Y., Inserra, C., Kankare, E., Kuncarayakti, H., Kouprianov, V., Kumar, Brajesh, Li, Xue, Lin, Han, Maguire, K., Mazzali, P., McCully, C., Milne, P., Mo, Jun, Morrell, N., Nicholl, M., Ochner, P., Olivares, F., Pastorello, A., Patat, F., Phillips, M., Pignata, G., Prentice, S., Reguitti, A., Reichart, D. E., Rodriguez, O., Rui, Liming, Sanwal, Pankaj, Sarneczky, K., Shahbandeh, M., Singh, Mridweeka, Smartt, S., Strader, J., Stritzinger, M. D., Szakats, R., Tartaglia, Leonardo, Wang, Huijuan, Wang, Lingzhi, Wang, Xiaofeng, Wheeler, J. C., Xiang, Danfeng, Yaron, O., Young, D. R., and Zhang, Junbo

Abstract

We present high-cadence UV, optical, and near-infrared data on the luminous Type II-P supernova SN;2017gmr from hours after discovery through the first 180 days. SN;2017gmr does not show signs of narrow, high-ionization emission lines in the early optical spectra, yet the optical light-curve evolution suggests that an extra energy source from circumstellar medium (CSM) interaction must be present for at least 2 days after explosion. Modeling of the early light curve indicates a ?500 R progenitor radius, consistent with a rather compact red supergiant, and late-time luminosities indicate that up to 0.130;;0.026 M of Ni-56 are present, if the light curve is solely powered by radioactive decay, although the Ni-56 mass may be lower if CSM interaction contributes to the post-plateau luminosity. Prominent multipeaked emission lines of H? and [O i] emerge after day 154, as a result of either an asymmetric explosion or asymmetries in the CSM. The lack of narrow lines within the first 2 days of explosion in the likely presence of CSM interaction may be an example of close, dense, asymmetric CSM that is quickly enveloped by the spherical supernova ejecta.

Published
2019
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4. SN 2015ba : a Type IIP supernova with a long plateau

Author

Dastidar, Raya, Misra, Kuntal, Hosseinzadeh, G., Pastorello, A., Pumo, M. L., Valenti, S., McCully, C., Tomasella, L., Arcavi, I, Elias-Rosa, N., Singh, Mridweeka, Gangopadhyay, Anjasha, Howell, D. A., Morales-Garoffolo, Antonia, Zampieri, L., Kumar, Brijesh, Turatto, M., Benetti, S., Tartaglia, Leonardo, Ochner, P., Sahu, D. K., Anupama, G. C., Pandey, S. B., Dastidar, Raya, Misra, Kuntal, Hosseinzadeh, G., Pastorello, A., Pumo, M. L., Valenti, S., McCully, C., Tomasella, L., Arcavi, I, Elias-Rosa, N., Singh, Mridweeka, Gangopadhyay, Anjasha, Howell, D. A., Morales-Garoffolo, Antonia, Zampieri, L., Kumar, Brijesh, Turatto, M., Benetti, S., Tartaglia, Leonardo, Ochner, P., Sahu, D. K., Anupama, G. C., and Pandey, S. B.

Abstract

We present optical photometry and spectroscopy from about a week after explosion to similar to 272 d of an atypical Type IIP supernova, SN 2015ba, which exploded in the edge-on galaxy IC 1029. SN 2015ba is a luminous event with an absolute V-band magnitude of -17.1 +/- 0.2 mag at 50 d since explosion and has a long plateau lasting for similar to 123 d. The distance to the SN is estimated to be 34.8 +/- 0.7 Mpc using the expanding photosphere and standard candle methods. High-velocity H Balmer components constant with time are observed in the late-plateau phase spectra of SN 2015ba, which suggests a possible role of circumstellar interaction at these phases. Both hydrodynamical and analytical modelling suggest a massive progenitor of SN 2015ba with a pre-explosion mass of 24-26 M-circle dot. However, the nebular spectra of SN 2015ba exhibit insignificant levels of oxygen, which is otherwise expected from a massive progenitor. This might be suggestive of the non-monotonical link between O-core masses and the zero-age main sequence mass of pre-supernova stars and/or uncertainties in the mixing scenario in the ejecta of supernovae.

Published
2018
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